2000 character limit reached
No massive black holes in the Milky Way halo (2403.02386v3)
Published 4 Mar 2024 in astro-ph.GA, astro-ph.CO, gr-qc, hep-ex, and hep-ph
Abstract: The gravitational wave detectors have unveiled a population of massive black holes that do not resemble those observed in the Milky Way and whose origin is debated. According to one possible explanation, these black holes may have formed from density fluctuations in the early Universe (primordial black holes), and they should comprise from several to 100% of dark matter to explain the observed black hole merger rates. If such black holes existed in the Milky Way dark matter halo, they would cause long-timescale gravitational microlensing events lasting years. The previous experiments were not sufficiently sensitive to such events. Here we present the results of the search for long-timescale microlensing events among the light curves of nearly 80 million stars located in the Large Magellanic Cloud that were monitored for 20 years by the OGLE survey. We did not find any events with timescales longer than one year, whereas all shorter events detected may be explained by known stellar populations. We find that compact objects in the mass range from $1.8 \times 10{-4}$ to $6.3\,M_{\odot}$ cannot compose more than 1% of dark matter, and those in the mass range from $1.3 \times 10{-5}$ to $860\,M_{\odot}$ cannot make up more than 10% of dark matter. Thus, primordial black holes in this mass range cannot simultaneously explain a significant fraction of dark matter and gravitational wave events.
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New limits from microlensing on Galactic black holes in the mass range 10 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT < M < 1000 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT. A&A 664, A106 (2022). [19] Udalski, A. The Optical Gravitational Lensing Experiment. Real Time Data Analysis Systems in the OGLE-III Survey. Acta Astron. 53, 291–305 (2003). [20] Mróz, P. et al. Microlensing optical depth and event rate toward the Large Magellanic Cloud based on 20 years of OGLE observations. submitted (2024). [21] Holtzman, J. A., Afonso, C. & Dolphin, A. The Local Group Stellar Populations Archive from the Hubble Space Telescope WFPC2. ApJS 166, 534–548 (2006). [22] Mróz, P. et al. No large population of unbound or wide-orbit Jupiter-mass planets. Nature 548, 183–186 (2017). [23] Cautun, M. et al. The milky way total mass profile as inferred from Gaia DR2. MNRAS 494, 4291–4313 (2020). [24] Han, C. & Gould, A. 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On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. A distance to the Large Magellanic Cloud that is precise to one per cent. Nature 567, 200–203 (2019). [42] Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. An H I Aperture Synthesis Mosaic of the Large Magellanic Cloud. ApJ 503, 674–688 (1998). [44] Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. The dark matter profile of the Milky Way inferred from its circular velocity curve. MNRAS 528, 693–710 (2024). [45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021). Abbott, B. P. et al. GWTC-1: A Gravitational-Wave Transient Catalog of Compact Binary Mergers Observed by LIGO and Virgo during the First and Second Observing Runs. Phys. Rev. X 9, 031040 (2019). [3] Abbott, R. et al. Population Properties of Compact Objects from the Second LIGO-Virgo Gravitational-Wave Transient Catalog. ApJ 913, L7 (2021). [4] Belczynski, K., Holz, D. E., Bulik, T. & O’Shaughnessy, R. The first gravitational-wave source from the isolated evolution of two stars in the 40-100 solar mass range. Nature 534, 512–515 (2016). [5] Askar, A., Szkudlarek, M., Gondek-Rosińska, D., Giersz, M. & Bulik, T. MOCCA-SURVEY Database - I. Coalescing binary black holes originating from globular clusters. MNRAS 464, L36–L40 (2017). [6] Rodriguez, C. L., Amaro-Seoane, P., Chatterjee, S. & Rasio, F. A. Post-Newtonian Dynamics in Dense Star Clusters: Highly Eccentric, Highly Spinning, and Repeated Binary Black Hole Mergers. Phys. Rev. Lett. 120, 151101 (2018). [7] Bird, S. et al. Did LIGO Detect Dark Matter? Phys. Rev. Lett. 116, 201301 (2016). [8] Sasaki, M., Suyama, T., Tanaka, T. & Yokoyama, S. Primordial Black Hole Scenario for the Gravitational-Wave Event GW150914. Phys. Rev. Lett. 117, 061101 (2016). [9] Clesse, S. & García-Bellido, J. The clustering of massive Primordial Black Holes as Dark Matter: Measuring their mass distribution with advanced LIGO. Phys. Dark Universe 15, 142–147 (2017). [10] Carr, B., Clesse, S., García-Bellido, J. & Kühnel, F. Cosmic conundra explained by thermal history and primordial black holes. Phys. Dark Universe 31, 100755 (2021). [11] Jedamzik, K. Consistency of Primordial Black Hole Dark Matter with LIGO/Virgo Merger Rates. Phys. Rev. Lett. 126, 051302 (2021). [12] Escrivà, A., Bagui, E. & Clesse, S. Simulations of PBH formation at the QCD epoch and comparison with the GWTC-3 catalog. J. Cosmology Astropart. Phys 2023, 004 (2023). [13] Udalski, A., Szymański, M. K. & Szymański, G. OGLE-IV: Fourth Phase of the Optical Gravitational Lensing Experiment. Acta Astron. 65, 1–38 (2015). [14] Paczyński, B. Gravitational microlensing by the galactic halo. ApJ 304, 1–5 (1986). [15] Alcock, C. et al. The MACHO Project: Microlensing Results from 5.7 Years of Large Magellanic Cloud Observations. ApJ 542, 281–307 (2000). [16] Tisserand, P. et al. Limits on the Macho content of the Galactic Halo from the EROS-2 Survey of the Magellanic Clouds. A&A 469, 387–404 (2007). [17] Wyrzykowski, L. et al. The OGLE view of microlensing towards the Magellanic Clouds - IV. OGLE-III SMC data and final conclusions on MACHOs. MNRAS 416, 2949–2961 (2011). [18] Blaineau, T. et al. New limits from microlensing on Galactic black holes in the mass range 10 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT < M < 1000 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT. A&A 664, A106 (2022). [19] Udalski, A. The Optical Gravitational Lensing Experiment. Real Time Data Analysis Systems in the OGLE-III Survey. Acta Astron. 53, 291–305 (2003). [20] Mróz, P. et al. Microlensing optical depth and event rate toward the Large Magellanic Cloud based on 20 years of OGLE observations. submitted (2024). [21] Holtzman, J. A., Afonso, C. & Dolphin, A. The Local Group Stellar Populations Archive from the Hubble Space Telescope WFPC2. ApJS 166, 534–548 (2006). [22] Mróz, P. et al. No large population of unbound or wide-orbit Jupiter-mass planets. Nature 548, 183–186 (2017). [23] Cautun, M. et al. The milky way total mass profile as inferred from Gaia DR2. MNRAS 494, 4291–4313 (2020). [24] Han, C. & Gould, A. Stellar Contribution to the Galactic Bulge Microlensing Optical Depth. ApJ 592, 172–175 (2003). [25] Niikura, H. et al. Microlensing constraints on primordial black holes with Subaru/HSC Andromeda observations. Nature Astronomy 3, 524–534 (2019). [26] Sahu, K. C. Stars within the Large Magellanic Cloud as potential lenses for observed microlensing events. Nature 370, 275–276 (1994). [27] Erkal, D. et al. The total mass of the Large Magellanic Cloud from its perturbation on the Orphan stream. MNRAS 487, 2685–2700 (2019). [28] Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. A&A 678, A208 (2023). [29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. A distance to the Large Magellanic Cloud that is precise to one per cent. Nature 567, 200–203 (2019). [42] Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. An H I Aperture Synthesis Mosaic of the Large Magellanic Cloud. ApJ 503, 674–688 (1998). [44] Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. The dark matter profile of the Milky Way inferred from its circular velocity curve. MNRAS 528, 693–710 (2024). [45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021). Abbott, R. et al. Population Properties of Compact Objects from the Second LIGO-Virgo Gravitational-Wave Transient Catalog. ApJ 913, L7 (2021). [4] Belczynski, K., Holz, D. E., Bulik, T. & O’Shaughnessy, R. The first gravitational-wave source from the isolated evolution of two stars in the 40-100 solar mass range. Nature 534, 512–515 (2016). [5] Askar, A., Szkudlarek, M., Gondek-Rosińska, D., Giersz, M. & Bulik, T. MOCCA-SURVEY Database - I. Coalescing binary black holes originating from globular clusters. MNRAS 464, L36–L40 (2017). [6] Rodriguez, C. L., Amaro-Seoane, P., Chatterjee, S. & Rasio, F. A. Post-Newtonian Dynamics in Dense Star Clusters: Highly Eccentric, Highly Spinning, and Repeated Binary Black Hole Mergers. Phys. Rev. Lett. 120, 151101 (2018). [7] Bird, S. et al. Did LIGO Detect Dark Matter? Phys. Rev. Lett. 116, 201301 (2016). [8] Sasaki, M., Suyama, T., Tanaka, T. & Yokoyama, S. Primordial Black Hole Scenario for the Gravitational-Wave Event GW150914. Phys. Rev. Lett. 117, 061101 (2016). [9] Clesse, S. & García-Bellido, J. The clustering of massive Primordial Black Holes as Dark Matter: Measuring their mass distribution with advanced LIGO. Phys. Dark Universe 15, 142–147 (2017). [10] Carr, B., Clesse, S., García-Bellido, J. & Kühnel, F. Cosmic conundra explained by thermal history and primordial black holes. Phys. Dark Universe 31, 100755 (2021). [11] Jedamzik, K. Consistency of Primordial Black Hole Dark Matter with LIGO/Virgo Merger Rates. Phys. Rev. Lett. 126, 051302 (2021). [12] Escrivà, A., Bagui, E. & Clesse, S. Simulations of PBH formation at the QCD epoch and comparison with the GWTC-3 catalog. J. Cosmology Astropart. Phys 2023, 004 (2023). [13] Udalski, A., Szymański, M. K. & Szymański, G. OGLE-IV: Fourth Phase of the Optical Gravitational Lensing Experiment. Acta Astron. 65, 1–38 (2015). [14] Paczyński, B. Gravitational microlensing by the galactic halo. ApJ 304, 1–5 (1986). [15] Alcock, C. et al. The MACHO Project: Microlensing Results from 5.7 Years of Large Magellanic Cloud Observations. ApJ 542, 281–307 (2000). [16] Tisserand, P. et al. Limits on the Macho content of the Galactic Halo from the EROS-2 Survey of the Magellanic Clouds. A&A 469, 387–404 (2007). [17] Wyrzykowski, L. et al. The OGLE view of microlensing towards the Magellanic Clouds - IV. OGLE-III SMC data and final conclusions on MACHOs. MNRAS 416, 2949–2961 (2011). [18] Blaineau, T. et al. New limits from microlensing on Galactic black holes in the mass range 10 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT < M < 1000 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT. A&A 664, A106 (2022). [19] Udalski, A. The Optical Gravitational Lensing Experiment. Real Time Data Analysis Systems in the OGLE-III Survey. Acta Astron. 53, 291–305 (2003). [20] Mróz, P. et al. Microlensing optical depth and event rate toward the Large Magellanic Cloud based on 20 years of OGLE observations. submitted (2024). [21] Holtzman, J. A., Afonso, C. & Dolphin, A. The Local Group Stellar Populations Archive from the Hubble Space Telescope WFPC2. ApJS 166, 534–548 (2006). [22] Mróz, P. et al. No large population of unbound or wide-orbit Jupiter-mass planets. Nature 548, 183–186 (2017). [23] Cautun, M. et al. The milky way total mass profile as inferred from Gaia DR2. MNRAS 494, 4291–4313 (2020). [24] Han, C. & Gould, A. Stellar Contribution to the Galactic Bulge Microlensing Optical Depth. ApJ 592, 172–175 (2003). [25] Niikura, H. et al. Microlensing constraints on primordial black holes with Subaru/HSC Andromeda observations. Nature Astronomy 3, 524–534 (2019). [26] Sahu, K. C. Stars within the Large Magellanic Cloud as potential lenses for observed microlensing events. Nature 370, 275–276 (1994). [27] Erkal, D. et al. The total mass of the Large Magellanic Cloud from its perturbation on the Orphan stream. MNRAS 487, 2685–2700 (2019). [28] Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. A&A 678, A208 (2023). [29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. A distance to the Large Magellanic Cloud that is precise to one per cent. Nature 567, 200–203 (2019). [42] Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. An H I Aperture Synthesis Mosaic of the Large Magellanic Cloud. ApJ 503, 674–688 (1998). [44] Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. The dark matter profile of the Milky Way inferred from its circular velocity curve. MNRAS 528, 693–710 (2024). [45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021). Belczynski, K., Holz, D. E., Bulik, T. & O’Shaughnessy, R. The first gravitational-wave source from the isolated evolution of two stars in the 40-100 solar mass range. Nature 534, 512–515 (2016). [5] Askar, A., Szkudlarek, M., Gondek-Rosińska, D., Giersz, M. & Bulik, T. MOCCA-SURVEY Database - I. Coalescing binary black holes originating from globular clusters. MNRAS 464, L36–L40 (2017). [6] Rodriguez, C. L., Amaro-Seoane, P., Chatterjee, S. & Rasio, F. A. Post-Newtonian Dynamics in Dense Star Clusters: Highly Eccentric, Highly Spinning, and Repeated Binary Black Hole Mergers. Phys. Rev. Lett. 120, 151101 (2018). [7] Bird, S. et al. Did LIGO Detect Dark Matter? Phys. Rev. Lett. 116, 201301 (2016). [8] Sasaki, M., Suyama, T., Tanaka, T. & Yokoyama, S. Primordial Black Hole Scenario for the Gravitational-Wave Event GW150914. Phys. Rev. Lett. 117, 061101 (2016). [9] Clesse, S. & García-Bellido, J. The clustering of massive Primordial Black Holes as Dark Matter: Measuring their mass distribution with advanced LIGO. Phys. Dark Universe 15, 142–147 (2017). [10] Carr, B., Clesse, S., García-Bellido, J. & Kühnel, F. Cosmic conundra explained by thermal history and primordial black holes. Phys. Dark Universe 31, 100755 (2021). [11] Jedamzik, K. Consistency of Primordial Black Hole Dark Matter with LIGO/Virgo Merger Rates. Phys. Rev. Lett. 126, 051302 (2021). [12] Escrivà, A., Bagui, E. & Clesse, S. Simulations of PBH formation at the QCD epoch and comparison with the GWTC-3 catalog. J. Cosmology Astropart. Phys 2023, 004 (2023). [13] Udalski, A., Szymański, M. K. & Szymański, G. OGLE-IV: Fourth Phase of the Optical Gravitational Lensing Experiment. Acta Astron. 65, 1–38 (2015). [14] Paczyński, B. Gravitational microlensing by the galactic halo. ApJ 304, 1–5 (1986). [15] Alcock, C. et al. The MACHO Project: Microlensing Results from 5.7 Years of Large Magellanic Cloud Observations. ApJ 542, 281–307 (2000). [16] Tisserand, P. et al. Limits on the Macho content of the Galactic Halo from the EROS-2 Survey of the Magellanic Clouds. A&A 469, 387–404 (2007). [17] Wyrzykowski, L. et al. The OGLE view of microlensing towards the Magellanic Clouds - IV. OGLE-III SMC data and final conclusions on MACHOs. MNRAS 416, 2949–2961 (2011). [18] Blaineau, T. et al. New limits from microlensing on Galactic black holes in the mass range 10 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT < M < 1000 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT. A&A 664, A106 (2022). [19] Udalski, A. The Optical Gravitational Lensing Experiment. Real Time Data Analysis Systems in the OGLE-III Survey. Acta Astron. 53, 291–305 (2003). [20] Mróz, P. et al. Microlensing optical depth and event rate toward the Large Magellanic Cloud based on 20 years of OGLE observations. submitted (2024). [21] Holtzman, J. A., Afonso, C. & Dolphin, A. The Local Group Stellar Populations Archive from the Hubble Space Telescope WFPC2. ApJS 166, 534–548 (2006). [22] Mróz, P. et al. No large population of unbound or wide-orbit Jupiter-mass planets. Nature 548, 183–186 (2017). [23] Cautun, M. et al. The milky way total mass profile as inferred from Gaia DR2. MNRAS 494, 4291–4313 (2020). [24] Han, C. & Gould, A. Stellar Contribution to the Galactic Bulge Microlensing Optical Depth. ApJ 592, 172–175 (2003). [25] Niikura, H. et al. Microlensing constraints on primordial black holes with Subaru/HSC Andromeda observations. Nature Astronomy 3, 524–534 (2019). [26] Sahu, K. C. Stars within the Large Magellanic Cloud as potential lenses for observed microlensing events. Nature 370, 275–276 (1994). [27] Erkal, D. et al. The total mass of the Large Magellanic Cloud from its perturbation on the Orphan stream. MNRAS 487, 2685–2700 (2019). [28] Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. A&A 678, A208 (2023). 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[34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. 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Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. 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ApJ 542, 281–307 (2000). [16] Tisserand, P. et al. Limits on the Macho content of the Galactic Halo from the EROS-2 Survey of the Magellanic Clouds. A&A 469, 387–404 (2007). [17] Wyrzykowski, L. et al. The OGLE view of microlensing towards the Magellanic Clouds - IV. OGLE-III SMC data and final conclusions on MACHOs. MNRAS 416, 2949–2961 (2011). [18] Blaineau, T. et al. New limits from microlensing on Galactic black holes in the mass range 10 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT < M < 1000 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT. A&A 664, A106 (2022). [19] Udalski, A. The Optical Gravitational Lensing Experiment. Real Time Data Analysis Systems in the OGLE-III Survey. Acta Astron. 53, 291–305 (2003). [20] Mróz, P. et al. Microlensing optical depth and event rate toward the Large Magellanic Cloud based on 20 years of OGLE observations. submitted (2024). [21] Holtzman, J. A., Afonso, C. & Dolphin, A. The Local Group Stellar Populations Archive from the Hubble Space Telescope WFPC2. ApJS 166, 534–548 (2006). [22] Mróz, P. et al. No large population of unbound or wide-orbit Jupiter-mass planets. Nature 548, 183–186 (2017). [23] Cautun, M. et al. The milky way total mass profile as inferred from Gaia DR2. MNRAS 494, 4291–4313 (2020). [24] Han, C. & Gould, A. Stellar Contribution to the Galactic Bulge Microlensing Optical Depth. ApJ 592, 172–175 (2003). [25] Niikura, H. et al. Microlensing constraints on primordial black holes with Subaru/HSC Andromeda observations. Nature Astronomy 3, 524–534 (2019). [26] Sahu, K. C. Stars within the Large Magellanic Cloud as potential lenses for observed microlensing events. Nature 370, 275–276 (1994). [27] Erkal, D. et al. The total mass of the Large Magellanic Cloud from its perturbation on the Orphan stream. MNRAS 487, 2685–2700 (2019). [28] Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. A&A 678, A208 (2023). [29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. A distance to the Large Magellanic Cloud that is precise to one per cent. Nature 567, 200–203 (2019). [42] Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. An H I Aperture Synthesis Mosaic of the Large Magellanic Cloud. ApJ 503, 674–688 (1998). [44] Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. The dark matter profile of the Milky Way inferred from its circular velocity curve. MNRAS 528, 693–710 (2024). [45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021). Clesse, S. & García-Bellido, J. The clustering of massive Primordial Black Holes as Dark Matter: Measuring their mass distribution with advanced LIGO. Phys. Dark Universe 15, 142–147 (2017). [10] Carr, B., Clesse, S., García-Bellido, J. & Kühnel, F. Cosmic conundra explained by thermal history and primordial black holes. Phys. Dark Universe 31, 100755 (2021). [11] Jedamzik, K. Consistency of Primordial Black Hole Dark Matter with LIGO/Virgo Merger Rates. Phys. Rev. Lett. 126, 051302 (2021). [12] Escrivà, A., Bagui, E. & Clesse, S. Simulations of PBH formation at the QCD epoch and comparison with the GWTC-3 catalog. J. Cosmology Astropart. Phys 2023, 004 (2023). [13] Udalski, A., Szymański, M. K. & Szymański, G. OGLE-IV: Fourth Phase of the Optical Gravitational Lensing Experiment. Acta Astron. 65, 1–38 (2015). [14] Paczyński, B. Gravitational microlensing by the galactic halo. ApJ 304, 1–5 (1986). [15] Alcock, C. et al. The MACHO Project: Microlensing Results from 5.7 Years of Large Magellanic Cloud Observations. ApJ 542, 281–307 (2000). [16] Tisserand, P. et al. Limits on the Macho content of the Galactic Halo from the EROS-2 Survey of the Magellanic Clouds. A&A 469, 387–404 (2007). [17] Wyrzykowski, L. et al. The OGLE view of microlensing towards the Magellanic Clouds - IV. OGLE-III SMC data and final conclusions on MACHOs. MNRAS 416, 2949–2961 (2011). [18] Blaineau, T. et al. New limits from microlensing on Galactic black holes in the mass range 10 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT < M < 1000 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT. A&A 664, A106 (2022). [19] Udalski, A. The Optical Gravitational Lensing Experiment. Real Time Data Analysis Systems in the OGLE-III Survey. Acta Astron. 53, 291–305 (2003). [20] Mróz, P. et al. Microlensing optical depth and event rate toward the Large Magellanic Cloud based on 20 years of OGLE observations. submitted (2024). [21] Holtzman, J. A., Afonso, C. & Dolphin, A. The Local Group Stellar Populations Archive from the Hubble Space Telescope WFPC2. ApJS 166, 534–548 (2006). [22] Mróz, P. et al. No large population of unbound or wide-orbit Jupiter-mass planets. Nature 548, 183–186 (2017). [23] Cautun, M. et al. The milky way total mass profile as inferred from Gaia DR2. MNRAS 494, 4291–4313 (2020). [24] Han, C. & Gould, A. Stellar Contribution to the Galactic Bulge Microlensing Optical Depth. ApJ 592, 172–175 (2003). [25] Niikura, H. et al. Microlensing constraints on primordial black holes with Subaru/HSC Andromeda observations. Nature Astronomy 3, 524–534 (2019). [26] Sahu, K. C. Stars within the Large Magellanic Cloud as potential lenses for observed microlensing events. Nature 370, 275–276 (1994). [27] Erkal, D. et al. The total mass of the Large Magellanic Cloud from its perturbation on the Orphan stream. MNRAS 487, 2685–2700 (2019). [28] Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. A&A 678, A208 (2023). [29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. A distance to the Large Magellanic Cloud that is precise to one per cent. Nature 567, 200–203 (2019). [42] Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. An H I Aperture Synthesis Mosaic of the Large Magellanic Cloud. ApJ 503, 674–688 (1998). [44] Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. The dark matter profile of the Milky Way inferred from its circular velocity curve. MNRAS 528, 693–710 (2024). [45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021). Carr, B., Clesse, S., García-Bellido, J. & Kühnel, F. Cosmic conundra explained by thermal history and primordial black holes. Phys. Dark Universe 31, 100755 (2021). [11] Jedamzik, K. Consistency of Primordial Black Hole Dark Matter with LIGO/Virgo Merger Rates. Phys. Rev. Lett. 126, 051302 (2021). [12] Escrivà, A., Bagui, E. & Clesse, S. Simulations of PBH formation at the QCD epoch and comparison with the GWTC-3 catalog. J. Cosmology Astropart. Phys 2023, 004 (2023). [13] Udalski, A., Szymański, M. K. & Szymański, G. OGLE-IV: Fourth Phase of the Optical Gravitational Lensing Experiment. Acta Astron. 65, 1–38 (2015). [14] Paczyński, B. Gravitational microlensing by the galactic halo. ApJ 304, 1–5 (1986). [15] Alcock, C. et al. The MACHO Project: Microlensing Results from 5.7 Years of Large Magellanic Cloud Observations. ApJ 542, 281–307 (2000). [16] Tisserand, P. et al. Limits on the Macho content of the Galactic Halo from the EROS-2 Survey of the Magellanic Clouds. A&A 469, 387–404 (2007). [17] Wyrzykowski, L. et al. The OGLE view of microlensing towards the Magellanic Clouds - IV. OGLE-III SMC data and final conclusions on MACHOs. MNRAS 416, 2949–2961 (2011). [18] Blaineau, T. et al. New limits from microlensing on Galactic black holes in the mass range 10 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT < M < 1000 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT. A&A 664, A106 (2022). [19] Udalski, A. The Optical Gravitational Lensing Experiment. Real Time Data Analysis Systems in the OGLE-III Survey. Acta Astron. 53, 291–305 (2003). [20] Mróz, P. et al. Microlensing optical depth and event rate toward the Large Magellanic Cloud based on 20 years of OGLE observations. submitted (2024). [21] Holtzman, J. A., Afonso, C. & Dolphin, A. The Local Group Stellar Populations Archive from the Hubble Space Telescope WFPC2. ApJS 166, 534–548 (2006). [22] Mróz, P. et al. No large population of unbound or wide-orbit Jupiter-mass planets. Nature 548, 183–186 (2017). [23] Cautun, M. et al. The milky way total mass profile as inferred from Gaia DR2. MNRAS 494, 4291–4313 (2020). [24] Han, C. & Gould, A. Stellar Contribution to the Galactic Bulge Microlensing Optical Depth. ApJ 592, 172–175 (2003). [25] Niikura, H. et al. Microlensing constraints on primordial black holes with Subaru/HSC Andromeda observations. Nature Astronomy 3, 524–534 (2019). [26] Sahu, K. C. Stars within the Large Magellanic Cloud as potential lenses for observed microlensing events. Nature 370, 275–276 (1994). [27] Erkal, D. et al. The total mass of the Large Magellanic Cloud from its perturbation on the Orphan stream. MNRAS 487, 2685–2700 (2019). [28] Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. A&A 678, A208 (2023). [29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. A distance to the Large Magellanic Cloud that is precise to one per cent. Nature 567, 200–203 (2019). [42] Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. An H I Aperture Synthesis Mosaic of the Large Magellanic Cloud. ApJ 503, 674–688 (1998). [44] Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. The dark matter profile of the Milky Way inferred from its circular velocity curve. MNRAS 528, 693–710 (2024). [45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021). Jedamzik, K. Consistency of Primordial Black Hole Dark Matter with LIGO/Virgo Merger Rates. Phys. Rev. Lett. 126, 051302 (2021). [12] Escrivà, A., Bagui, E. & Clesse, S. Simulations of PBH formation at the QCD epoch and comparison with the GWTC-3 catalog. J. Cosmology Astropart. Phys 2023, 004 (2023). [13] Udalski, A., Szymański, M. K. & Szymański, G. OGLE-IV: Fourth Phase of the Optical Gravitational Lensing Experiment. Acta Astron. 65, 1–38 (2015). [14] Paczyński, B. Gravitational microlensing by the galactic halo. ApJ 304, 1–5 (1986). [15] Alcock, C. et al. The MACHO Project: Microlensing Results from 5.7 Years of Large Magellanic Cloud Observations. ApJ 542, 281–307 (2000). [16] Tisserand, P. et al. Limits on the Macho content of the Galactic Halo from the EROS-2 Survey of the Magellanic Clouds. A&A 469, 387–404 (2007). [17] Wyrzykowski, L. et al. The OGLE view of microlensing towards the Magellanic Clouds - IV. OGLE-III SMC data and final conclusions on MACHOs. MNRAS 416, 2949–2961 (2011). [18] Blaineau, T. et al. New limits from microlensing on Galactic black holes in the mass range 10 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT < M < 1000 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT. A&A 664, A106 (2022). [19] Udalski, A. The Optical Gravitational Lensing Experiment. Real Time Data Analysis Systems in the OGLE-III Survey. Acta Astron. 53, 291–305 (2003). [20] Mróz, P. et al. Microlensing optical depth and event rate toward the Large Magellanic Cloud based on 20 years of OGLE observations. submitted (2024). [21] Holtzman, J. A., Afonso, C. & Dolphin, A. The Local Group Stellar Populations Archive from the Hubble Space Telescope WFPC2. ApJS 166, 534–548 (2006). [22] Mróz, P. et al. No large population of unbound or wide-orbit Jupiter-mass planets. Nature 548, 183–186 (2017). [23] Cautun, M. et al. The milky way total mass profile as inferred from Gaia DR2. MNRAS 494, 4291–4313 (2020). [24] Han, C. & Gould, A. Stellar Contribution to the Galactic Bulge Microlensing Optical Depth. ApJ 592, 172–175 (2003). [25] Niikura, H. et al. Microlensing constraints on primordial black holes with Subaru/HSC Andromeda observations. Nature Astronomy 3, 524–534 (2019). [26] Sahu, K. C. Stars within the Large Magellanic Cloud as potential lenses for observed microlensing events. Nature 370, 275–276 (1994). [27] Erkal, D. et al. The total mass of the Large Magellanic Cloud from its perturbation on the Orphan stream. MNRAS 487, 2685–2700 (2019). [28] Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. A&A 678, A208 (2023). [29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. A distance to the Large Magellanic Cloud that is precise to one per cent. Nature 567, 200–203 (2019). [42] Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. An H I Aperture Synthesis Mosaic of the Large Magellanic Cloud. ApJ 503, 674–688 (1998). [44] Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. The dark matter profile of the Milky Way inferred from its circular velocity curve. MNRAS 528, 693–710 (2024). [45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021). Escrivà, A., Bagui, E. & Clesse, S. Simulations of PBH formation at the QCD epoch and comparison with the GWTC-3 catalog. J. Cosmology Astropart. Phys 2023, 004 (2023). [13] Udalski, A., Szymański, M. K. & Szymański, G. OGLE-IV: Fourth Phase of the Optical Gravitational Lensing Experiment. Acta Astron. 65, 1–38 (2015). [14] Paczyński, B. Gravitational microlensing by the galactic halo. ApJ 304, 1–5 (1986). [15] Alcock, C. et al. The MACHO Project: Microlensing Results from 5.7 Years of Large Magellanic Cloud Observations. ApJ 542, 281–307 (2000). [16] Tisserand, P. et al. Limits on the Macho content of the Galactic Halo from the EROS-2 Survey of the Magellanic Clouds. A&A 469, 387–404 (2007). [17] Wyrzykowski, L. et al. The OGLE view of microlensing towards the Magellanic Clouds - IV. OGLE-III SMC data and final conclusions on MACHOs. MNRAS 416, 2949–2961 (2011). [18] Blaineau, T. et al. New limits from microlensing on Galactic black holes in the mass range 10 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT < M < 1000 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT. A&A 664, A106 (2022). [19] Udalski, A. The Optical Gravitational Lensing Experiment. Real Time Data Analysis Systems in the OGLE-III Survey. Acta Astron. 53, 291–305 (2003). [20] Mróz, P. et al. Microlensing optical depth and event rate toward the Large Magellanic Cloud based on 20 years of OGLE observations. submitted (2024). [21] Holtzman, J. A., Afonso, C. & Dolphin, A. The Local Group Stellar Populations Archive from the Hubble Space Telescope WFPC2. ApJS 166, 534–548 (2006). [22] Mróz, P. et al. No large population of unbound or wide-orbit Jupiter-mass planets. Nature 548, 183–186 (2017). [23] Cautun, M. et al. The milky way total mass profile as inferred from Gaia DR2. MNRAS 494, 4291–4313 (2020). [24] Han, C. & Gould, A. Stellar Contribution to the Galactic Bulge Microlensing Optical Depth. ApJ 592, 172–175 (2003). [25] Niikura, H. et al. Microlensing constraints on primordial black holes with Subaru/HSC Andromeda observations. Nature Astronomy 3, 524–534 (2019). [26] Sahu, K. C. Stars within the Large Magellanic Cloud as potential lenses for observed microlensing events. Nature 370, 275–276 (1994). [27] Erkal, D. et al. The total mass of the Large Magellanic Cloud from its perturbation on the Orphan stream. MNRAS 487, 2685–2700 (2019). [28] Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. A&A 678, A208 (2023). [29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. A distance to the Large Magellanic Cloud that is precise to one per cent. Nature 567, 200–203 (2019). [42] Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. An H I Aperture Synthesis Mosaic of the Large Magellanic Cloud. ApJ 503, 674–688 (1998). [44] Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. The dark matter profile of the Milky Way inferred from its circular velocity curve. MNRAS 528, 693–710 (2024). [45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021). Udalski, A., Szymański, M. K. & Szymański, G. OGLE-IV: Fourth Phase of the Optical Gravitational Lensing Experiment. Acta Astron. 65, 1–38 (2015). [14] Paczyński, B. Gravitational microlensing by the galactic halo. ApJ 304, 1–5 (1986). [15] Alcock, C. et al. The MACHO Project: Microlensing Results from 5.7 Years of Large Magellanic Cloud Observations. ApJ 542, 281–307 (2000). [16] Tisserand, P. et al. Limits on the Macho content of the Galactic Halo from the EROS-2 Survey of the Magellanic Clouds. A&A 469, 387–404 (2007). [17] Wyrzykowski, L. et al. The OGLE view of microlensing towards the Magellanic Clouds - IV. OGLE-III SMC data and final conclusions on MACHOs. MNRAS 416, 2949–2961 (2011). [18] Blaineau, T. et al. New limits from microlensing on Galactic black holes in the mass range 10 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT < M < 1000 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT. A&A 664, A106 (2022). [19] Udalski, A. The Optical Gravitational Lensing Experiment. Real Time Data Analysis Systems in the OGLE-III Survey. Acta Astron. 53, 291–305 (2003). [20] Mróz, P. et al. Microlensing optical depth and event rate toward the Large Magellanic Cloud based on 20 years of OGLE observations. submitted (2024). [21] Holtzman, J. A., Afonso, C. & Dolphin, A. The Local Group Stellar Populations Archive from the Hubble Space Telescope WFPC2. ApJS 166, 534–548 (2006). [22] Mróz, P. et al. No large population of unbound or wide-orbit Jupiter-mass planets. Nature 548, 183–186 (2017). [23] Cautun, M. et al. The milky way total mass profile as inferred from Gaia DR2. MNRAS 494, 4291–4313 (2020). [24] Han, C. & Gould, A. Stellar Contribution to the Galactic Bulge Microlensing Optical Depth. ApJ 592, 172–175 (2003). [25] Niikura, H. et al. Microlensing constraints on primordial black holes with Subaru/HSC Andromeda observations. Nature Astronomy 3, 524–534 (2019). [26] Sahu, K. C. Stars within the Large Magellanic Cloud as potential lenses for observed microlensing events. Nature 370, 275–276 (1994). [27] Erkal, D. et al. The total mass of the Large Magellanic Cloud from its perturbation on the Orphan stream. MNRAS 487, 2685–2700 (2019). [28] Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. A&A 678, A208 (2023). [29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. A distance to the Large Magellanic Cloud that is precise to one per cent. Nature 567, 200–203 (2019). [42] Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. An H I Aperture Synthesis Mosaic of the Large Magellanic Cloud. ApJ 503, 674–688 (1998). [44] Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. The dark matter profile of the Milky Way inferred from its circular velocity curve. MNRAS 528, 693–710 (2024). [45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021). Paczyński, B. Gravitational microlensing by the galactic halo. ApJ 304, 1–5 (1986). [15] Alcock, C. et al. The MACHO Project: Microlensing Results from 5.7 Years of Large Magellanic Cloud Observations. ApJ 542, 281–307 (2000). [16] Tisserand, P. et al. Limits on the Macho content of the Galactic Halo from the EROS-2 Survey of the Magellanic Clouds. A&A 469, 387–404 (2007). [17] Wyrzykowski, L. et al. The OGLE view of microlensing towards the Magellanic Clouds - IV. OGLE-III SMC data and final conclusions on MACHOs. MNRAS 416, 2949–2961 (2011). [18] Blaineau, T. et al. New limits from microlensing on Galactic black holes in the mass range 10 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT < M < 1000 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT. A&A 664, A106 (2022). [19] Udalski, A. The Optical Gravitational Lensing Experiment. Real Time Data Analysis Systems in the OGLE-III Survey. Acta Astron. 53, 291–305 (2003). [20] Mróz, P. et al. Microlensing optical depth and event rate toward the Large Magellanic Cloud based on 20 years of OGLE observations. submitted (2024). [21] Holtzman, J. A., Afonso, C. & Dolphin, A. The Local Group Stellar Populations Archive from the Hubble Space Telescope WFPC2. ApJS 166, 534–548 (2006). [22] Mróz, P. et al. No large population of unbound or wide-orbit Jupiter-mass planets. Nature 548, 183–186 (2017). [23] Cautun, M. et al. The milky way total mass profile as inferred from Gaia DR2. MNRAS 494, 4291–4313 (2020). [24] Han, C. & Gould, A. Stellar Contribution to the Galactic Bulge Microlensing Optical Depth. ApJ 592, 172–175 (2003). [25] Niikura, H. et al. Microlensing constraints on primordial black holes with Subaru/HSC Andromeda observations. Nature Astronomy 3, 524–534 (2019). [26] Sahu, K. C. Stars within the Large Magellanic Cloud as potential lenses for observed microlensing events. Nature 370, 275–276 (1994). [27] Erkal, D. et al. The total mass of the Large Magellanic Cloud from its perturbation on the Orphan stream. MNRAS 487, 2685–2700 (2019). [28] Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. A&A 678, A208 (2023). [29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. A distance to the Large Magellanic Cloud that is precise to one per cent. Nature 567, 200–203 (2019). [42] Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. An H I Aperture Synthesis Mosaic of the Large Magellanic Cloud. ApJ 503, 674–688 (1998). [44] Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. The dark matter profile of the Milky Way inferred from its circular velocity curve. MNRAS 528, 693–710 (2024). [45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021). Alcock, C. et al. The MACHO Project: Microlensing Results from 5.7 Years of Large Magellanic Cloud Observations. ApJ 542, 281–307 (2000). [16] Tisserand, P. et al. Limits on the Macho content of the Galactic Halo from the EROS-2 Survey of the Magellanic Clouds. A&A 469, 387–404 (2007). [17] Wyrzykowski, L. et al. The OGLE view of microlensing towards the Magellanic Clouds - IV. OGLE-III SMC data and final conclusions on MACHOs. MNRAS 416, 2949–2961 (2011). [18] Blaineau, T. et al. New limits from microlensing on Galactic black holes in the mass range 10 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT < M < 1000 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT. A&A 664, A106 (2022). [19] Udalski, A. The Optical Gravitational Lensing Experiment. Real Time Data Analysis Systems in the OGLE-III Survey. Acta Astron. 53, 291–305 (2003). [20] Mróz, P. et al. Microlensing optical depth and event rate toward the Large Magellanic Cloud based on 20 years of OGLE observations. submitted (2024). [21] Holtzman, J. A., Afonso, C. & Dolphin, A. The Local Group Stellar Populations Archive from the Hubble Space Telescope WFPC2. ApJS 166, 534–548 (2006). [22] Mróz, P. et al. No large population of unbound or wide-orbit Jupiter-mass planets. Nature 548, 183–186 (2017). [23] Cautun, M. et al. The milky way total mass profile as inferred from Gaia DR2. MNRAS 494, 4291–4313 (2020). [24] Han, C. & Gould, A. Stellar Contribution to the Galactic Bulge Microlensing Optical Depth. ApJ 592, 172–175 (2003). [25] Niikura, H. et al. Microlensing constraints on primordial black holes with Subaru/HSC Andromeda observations. Nature Astronomy 3, 524–534 (2019). [26] Sahu, K. C. Stars within the Large Magellanic Cloud as potential lenses for observed microlensing events. Nature 370, 275–276 (1994). [27] Erkal, D. et al. The total mass of the Large Magellanic Cloud from its perturbation on the Orphan stream. MNRAS 487, 2685–2700 (2019). [28] Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. A&A 678, A208 (2023). [29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. A distance to the Large Magellanic Cloud that is precise to one per cent. Nature 567, 200–203 (2019). [42] Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. An H I Aperture Synthesis Mosaic of the Large Magellanic Cloud. ApJ 503, 674–688 (1998). [44] Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. The dark matter profile of the Milky Way inferred from its circular velocity curve. MNRAS 528, 693–710 (2024). [45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021). Tisserand, P. et al. Limits on the Macho content of the Galactic Halo from the EROS-2 Survey of the Magellanic Clouds. A&A 469, 387–404 (2007). [17] Wyrzykowski, L. et al. The OGLE view of microlensing towards the Magellanic Clouds - IV. OGLE-III SMC data and final conclusions on MACHOs. MNRAS 416, 2949–2961 (2011). [18] Blaineau, T. et al. New limits from microlensing on Galactic black holes in the mass range 10 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT < M < 1000 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT. A&A 664, A106 (2022). [19] Udalski, A. The Optical Gravitational Lensing Experiment. Real Time Data Analysis Systems in the OGLE-III Survey. Acta Astron. 53, 291–305 (2003). [20] Mróz, P. et al. Microlensing optical depth and event rate toward the Large Magellanic Cloud based on 20 years of OGLE observations. submitted (2024). [21] Holtzman, J. A., Afonso, C. & Dolphin, A. The Local Group Stellar Populations Archive from the Hubble Space Telescope WFPC2. ApJS 166, 534–548 (2006). [22] Mróz, P. et al. No large population of unbound or wide-orbit Jupiter-mass planets. Nature 548, 183–186 (2017). [23] Cautun, M. et al. The milky way total mass profile as inferred from Gaia DR2. MNRAS 494, 4291–4313 (2020). [24] Han, C. & Gould, A. Stellar Contribution to the Galactic Bulge Microlensing Optical Depth. ApJ 592, 172–175 (2003). [25] Niikura, H. et al. Microlensing constraints on primordial black holes with Subaru/HSC Andromeda observations. Nature Astronomy 3, 524–534 (2019). [26] Sahu, K. C. Stars within the Large Magellanic Cloud as potential lenses for observed microlensing events. Nature 370, 275–276 (1994). [27] Erkal, D. et al. The total mass of the Large Magellanic Cloud from its perturbation on the Orphan stream. MNRAS 487, 2685–2700 (2019). [28] Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. A&A 678, A208 (2023). [29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. A distance to the Large Magellanic Cloud that is precise to one per cent. Nature 567, 200–203 (2019). [42] Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. An H I Aperture Synthesis Mosaic of the Large Magellanic Cloud. ApJ 503, 674–688 (1998). [44] Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. The dark matter profile of the Milky Way inferred from its circular velocity curve. MNRAS 528, 693–710 (2024). [45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021). Wyrzykowski, L. et al. The OGLE view of microlensing towards the Magellanic Clouds - IV. OGLE-III SMC data and final conclusions on MACHOs. MNRAS 416, 2949–2961 (2011). [18] Blaineau, T. et al. New limits from microlensing on Galactic black holes in the mass range 10 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT < M < 1000 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT. A&A 664, A106 (2022). [19] Udalski, A. The Optical Gravitational Lensing Experiment. Real Time Data Analysis Systems in the OGLE-III Survey. Acta Astron. 53, 291–305 (2003). [20] Mróz, P. et al. Microlensing optical depth and event rate toward the Large Magellanic Cloud based on 20 years of OGLE observations. submitted (2024). [21] Holtzman, J. A., Afonso, C. & Dolphin, A. The Local Group Stellar Populations Archive from the Hubble Space Telescope WFPC2. ApJS 166, 534–548 (2006). [22] Mróz, P. et al. No large population of unbound or wide-orbit Jupiter-mass planets. Nature 548, 183–186 (2017). [23] Cautun, M. et al. The milky way total mass profile as inferred from Gaia DR2. MNRAS 494, 4291–4313 (2020). [24] Han, C. & Gould, A. Stellar Contribution to the Galactic Bulge Microlensing Optical Depth. ApJ 592, 172–175 (2003). [25] Niikura, H. et al. Microlensing constraints on primordial black holes with Subaru/HSC Andromeda observations. Nature Astronomy 3, 524–534 (2019). [26] Sahu, K. C. Stars within the Large Magellanic Cloud as potential lenses for observed microlensing events. Nature 370, 275–276 (1994). [27] Erkal, D. et al. The total mass of the Large Magellanic Cloud from its perturbation on the Orphan stream. MNRAS 487, 2685–2700 (2019). [28] Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. A&A 678, A208 (2023). [29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. A distance to the Large Magellanic Cloud that is precise to one per cent. Nature 567, 200–203 (2019). [42] Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. An H I Aperture Synthesis Mosaic of the Large Magellanic Cloud. ApJ 503, 674–688 (1998). [44] Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. The dark matter profile of the Milky Way inferred from its circular velocity curve. MNRAS 528, 693–710 (2024). [45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021). Blaineau, T. et al. New limits from microlensing on Galactic black holes in the mass range 10 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT < M < 1000 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT. A&A 664, A106 (2022). [19] Udalski, A. The Optical Gravitational Lensing Experiment. Real Time Data Analysis Systems in the OGLE-III Survey. Acta Astron. 53, 291–305 (2003). [20] Mróz, P. et al. 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The total mass of the Large Magellanic Cloud from its perturbation on the Orphan stream. MNRAS 487, 2685–2700 (2019). [28] Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. A&A 678, A208 (2023). [29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. A distance to the Large Magellanic Cloud that is precise to one per cent. Nature 567, 200–203 (2019). [42] Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. An H I Aperture Synthesis Mosaic of the Large Magellanic Cloud. ApJ 503, 674–688 (1998). [44] Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. The dark matter profile of the Milky Way inferred from its circular velocity curve. MNRAS 528, 693–710 (2024). [45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021). Udalski, A. The Optical Gravitational Lensing Experiment. Real Time Data Analysis Systems in the OGLE-III Survey. Acta Astron. 53, 291–305 (2003). [20] Mróz, P. et al. 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The total mass of the Large Magellanic Cloud from its perturbation on the Orphan stream. MNRAS 487, 2685–2700 (2019). [28] Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. A&A 678, A208 (2023). [29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. 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The Local Group Stellar Populations Archive from the Hubble Space Telescope WFPC2. ApJS 166, 534–548 (2006). [22] Mróz, P. et al. No large population of unbound or wide-orbit Jupiter-mass planets. Nature 548, 183–186 (2017). [23] Cautun, M. et al. The milky way total mass profile as inferred from Gaia DR2. MNRAS 494, 4291–4313 (2020). [24] Han, C. & Gould, A. Stellar Contribution to the Galactic Bulge Microlensing Optical Depth. ApJ 592, 172–175 (2003). [25] Niikura, H. et al. Microlensing constraints on primordial black holes with Subaru/HSC Andromeda observations. Nature Astronomy 3, 524–534 (2019). [26] Sahu, K. C. Stars within the Large Magellanic Cloud as potential lenses for observed microlensing events. Nature 370, 275–276 (1994). [27] Erkal, D. et al. The total mass of the Large Magellanic Cloud from its perturbation on the Orphan stream. MNRAS 487, 2685–2700 (2019). [28] Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. A&A 678, A208 (2023). [29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. A distance to the Large Magellanic Cloud that is precise to one per cent. Nature 567, 200–203 (2019). [42] Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. An H I Aperture Synthesis Mosaic of the Large Magellanic Cloud. ApJ 503, 674–688 (1998). [44] Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. The dark matter profile of the Milky Way inferred from its circular velocity curve. MNRAS 528, 693–710 (2024). [45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021). Holtzman, J. A., Afonso, C. & Dolphin, A. The Local Group Stellar Populations Archive from the Hubble Space Telescope WFPC2. ApJS 166, 534–548 (2006). [22] Mróz, P. et al. No large population of unbound or wide-orbit Jupiter-mass planets. Nature 548, 183–186 (2017). [23] Cautun, M. et al. The milky way total mass profile as inferred from Gaia DR2. MNRAS 494, 4291–4313 (2020). [24] Han, C. & Gould, A. Stellar Contribution to the Galactic Bulge Microlensing Optical Depth. ApJ 592, 172–175 (2003). [25] Niikura, H. et al. Microlensing constraints on primordial black holes with Subaru/HSC Andromeda observations. Nature Astronomy 3, 524–534 (2019). [26] Sahu, K. C. Stars within the Large Magellanic Cloud as potential lenses for observed microlensing events. Nature 370, 275–276 (1994). [27] Erkal, D. et al. The total mass of the Large Magellanic Cloud from its perturbation on the Orphan stream. MNRAS 487, 2685–2700 (2019). [28] Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. A&A 678, A208 (2023). [29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. A distance to the Large Magellanic Cloud that is precise to one per cent. Nature 567, 200–203 (2019). [42] Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. An H I Aperture Synthesis Mosaic of the Large Magellanic Cloud. ApJ 503, 674–688 (1998). [44] Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. The dark matter profile of the Milky Way inferred from its circular velocity curve. MNRAS 528, 693–710 (2024). [45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. 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Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. A distance to the Large Magellanic Cloud that is precise to one per cent. Nature 567, 200–203 (2019). [42] Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. An H I Aperture Synthesis Mosaic of the Large Magellanic Cloud. ApJ 503, 674–688 (1998). [44] Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. The dark matter profile of the Milky Way inferred from its circular velocity curve. MNRAS 528, 693–710 (2024). [45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021). Cautun, M. et al. The milky way total mass profile as inferred from Gaia DR2. MNRAS 494, 4291–4313 (2020). [24] Han, C. & Gould, A. Stellar Contribution to the Galactic Bulge Microlensing Optical Depth. ApJ 592, 172–175 (2003). [25] Niikura, H. et al. Microlensing constraints on primordial black holes with Subaru/HSC Andromeda observations. Nature Astronomy 3, 524–534 (2019). [26] Sahu, K. C. Stars within the Large Magellanic Cloud as potential lenses for observed microlensing events. Nature 370, 275–276 (1994). [27] Erkal, D. et al. The total mass of the Large Magellanic Cloud from its perturbation on the Orphan stream. MNRAS 487, 2685–2700 (2019). [28] Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. A&A 678, A208 (2023). [29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. A distance to the Large Magellanic Cloud that is precise to one per cent. Nature 567, 200–203 (2019). [42] Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. An H I Aperture Synthesis Mosaic of the Large Magellanic Cloud. ApJ 503, 674–688 (1998). [44] Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. The dark matter profile of the Milky Way inferred from its circular velocity curve. MNRAS 528, 693–710 (2024). [45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021). Han, C. & Gould, A. Stellar Contribution to the Galactic Bulge Microlensing Optical Depth. ApJ 592, 172–175 (2003). [25] Niikura, H. et al. Microlensing constraints on primordial black holes with Subaru/HSC Andromeda observations. Nature Astronomy 3, 524–534 (2019). 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The total mass of the Large Magellanic Cloud from its perturbation on the Orphan stream. MNRAS 487, 2685–2700 (2019). [28] Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. A&A 678, A208 (2023). [29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. 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[9] Clesse, S. & García-Bellido, J. The clustering of massive Primordial Black Holes as Dark Matter: Measuring their mass distribution with advanced LIGO. Phys. Dark Universe 15, 142–147 (2017). [10] Carr, B., Clesse, S., García-Bellido, J. & Kühnel, F. Cosmic conundra explained by thermal history and primordial black holes. Phys. Dark Universe 31, 100755 (2021). [11] Jedamzik, K. Consistency of Primordial Black Hole Dark Matter with LIGO/Virgo Merger Rates. Phys. Rev. Lett. 126, 051302 (2021). [12] Escrivà, A., Bagui, E. & Clesse, S. Simulations of PBH formation at the QCD epoch and comparison with the GWTC-3 catalog. J. Cosmology Astropart. Phys 2023, 004 (2023). [13] Udalski, A., Szymański, M. K. & Szymański, G. OGLE-IV: Fourth Phase of the Optical Gravitational Lensing Experiment. Acta Astron. 65, 1–38 (2015). [14] Paczyński, B. Gravitational microlensing by the galactic halo. ApJ 304, 1–5 (1986). [15] Alcock, C. et al. The MACHO Project: Microlensing Results from 5.7 Years of Large Magellanic Cloud Observations. ApJ 542, 281–307 (2000). [16] Tisserand, P. et al. Limits on the Macho content of the Galactic Halo from the EROS-2 Survey of the Magellanic Clouds. A&A 469, 387–404 (2007). [17] Wyrzykowski, L. et al. The OGLE view of microlensing towards the Magellanic Clouds - IV. OGLE-III SMC data and final conclusions on MACHOs. MNRAS 416, 2949–2961 (2011). [18] Blaineau, T. et al. New limits from microlensing on Galactic black holes in the mass range 10 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT < M < 1000 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT. A&A 664, A106 (2022). [19] Udalski, A. The Optical Gravitational Lensing Experiment. Real Time Data Analysis Systems in the OGLE-III Survey. Acta Astron. 53, 291–305 (2003). [20] Mróz, P. et al. Microlensing optical depth and event rate toward the Large Magellanic Cloud based on 20 years of OGLE observations. submitted (2024). [21] Holtzman, J. A., Afonso, C. & Dolphin, A. The Local Group Stellar Populations Archive from the Hubble Space Telescope WFPC2. ApJS 166, 534–548 (2006). [22] Mróz, P. et al. No large population of unbound or wide-orbit Jupiter-mass planets. Nature 548, 183–186 (2017). [23] Cautun, M. et al. The milky way total mass profile as inferred from Gaia DR2. MNRAS 494, 4291–4313 (2020). [24] Han, C. & Gould, A. Stellar Contribution to the Galactic Bulge Microlensing Optical Depth. ApJ 592, 172–175 (2003). [25] Niikura, H. et al. Microlensing constraints on primordial black holes with Subaru/HSC Andromeda observations. Nature Astronomy 3, 524–534 (2019). [26] Sahu, K. C. Stars within the Large Magellanic Cloud as potential lenses for observed microlensing events. Nature 370, 275–276 (1994). [27] Erkal, D. et al. The total mass of the Large Magellanic Cloud from its perturbation on the Orphan stream. MNRAS 487, 2685–2700 (2019). [28] Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. A&A 678, A208 (2023). [29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. A distance to the Large Magellanic Cloud that is precise to one per cent. Nature 567, 200–203 (2019). [42] Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. An H I Aperture Synthesis Mosaic of the Large Magellanic Cloud. ApJ 503, 674–688 (1998). [44] Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. The dark matter profile of the Milky Way inferred from its circular velocity curve. MNRAS 528, 693–710 (2024). [45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021). Sasaki, M., Suyama, T., Tanaka, T. & Yokoyama, S. Primordial Black Hole Scenario for the Gravitational-Wave Event GW150914. Phys. Rev. Lett. 117, 061101 (2016). [9] Clesse, S. & García-Bellido, J. The clustering of massive Primordial Black Holes as Dark Matter: Measuring their mass distribution with advanced LIGO. Phys. Dark Universe 15, 142–147 (2017). [10] Carr, B., Clesse, S., García-Bellido, J. & Kühnel, F. Cosmic conundra explained by thermal history and primordial black holes. Phys. Dark Universe 31, 100755 (2021). [11] Jedamzik, K. Consistency of Primordial Black Hole Dark Matter with LIGO/Virgo Merger Rates. Phys. Rev. Lett. 126, 051302 (2021). [12] Escrivà, A., Bagui, E. & Clesse, S. Simulations of PBH formation at the QCD epoch and comparison with the GWTC-3 catalog. J. Cosmology Astropart. Phys 2023, 004 (2023). [13] Udalski, A., Szymański, M. K. & Szymański, G. OGLE-IV: Fourth Phase of the Optical Gravitational Lensing Experiment. Acta Astron. 65, 1–38 (2015). [14] Paczyński, B. Gravitational microlensing by the galactic halo. ApJ 304, 1–5 (1986). [15] Alcock, C. et al. The MACHO Project: Microlensing Results from 5.7 Years of Large Magellanic Cloud Observations. ApJ 542, 281–307 (2000). [16] Tisserand, P. et al. Limits on the Macho content of the Galactic Halo from the EROS-2 Survey of the Magellanic Clouds. A&A 469, 387–404 (2007). [17] Wyrzykowski, L. et al. The OGLE view of microlensing towards the Magellanic Clouds - IV. OGLE-III SMC data and final conclusions on MACHOs. MNRAS 416, 2949–2961 (2011). [18] Blaineau, T. et al. New limits from microlensing on Galactic black holes in the mass range 10 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT < M < 1000 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT. A&A 664, A106 (2022). [19] Udalski, A. The Optical Gravitational Lensing Experiment. Real Time Data Analysis Systems in the OGLE-III Survey. Acta Astron. 53, 291–305 (2003). [20] Mróz, P. et al. Microlensing optical depth and event rate toward the Large Magellanic Cloud based on 20 years of OGLE observations. submitted (2024). [21] Holtzman, J. A., Afonso, C. & Dolphin, A. The Local Group Stellar Populations Archive from the Hubble Space Telescope WFPC2. ApJS 166, 534–548 (2006). [22] Mróz, P. et al. No large population of unbound or wide-orbit Jupiter-mass planets. Nature 548, 183–186 (2017). [23] Cautun, M. et al. The milky way total mass profile as inferred from Gaia DR2. MNRAS 494, 4291–4313 (2020). [24] Han, C. & Gould, A. Stellar Contribution to the Galactic Bulge Microlensing Optical Depth. ApJ 592, 172–175 (2003). [25] Niikura, H. et al. Microlensing constraints on primordial black holes with Subaru/HSC Andromeda observations. Nature Astronomy 3, 524–534 (2019). [26] Sahu, K. C. Stars within the Large Magellanic Cloud as potential lenses for observed microlensing events. Nature 370, 275–276 (1994). [27] Erkal, D. et al. The total mass of the Large Magellanic Cloud from its perturbation on the Orphan stream. MNRAS 487, 2685–2700 (2019). [28] Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. A&A 678, A208 (2023). [29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. A distance to the Large Magellanic Cloud that is precise to one per cent. Nature 567, 200–203 (2019). [42] Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. An H I Aperture Synthesis Mosaic of the Large Magellanic Cloud. ApJ 503, 674–688 (1998). [44] Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. The dark matter profile of the Milky Way inferred from its circular velocity curve. MNRAS 528, 693–710 (2024). [45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021). Clesse, S. & García-Bellido, J. The clustering of massive Primordial Black Holes as Dark Matter: Measuring their mass distribution with advanced LIGO. Phys. Dark Universe 15, 142–147 (2017). [10] Carr, B., Clesse, S., García-Bellido, J. & Kühnel, F. Cosmic conundra explained by thermal history and primordial black holes. Phys. Dark Universe 31, 100755 (2021). [11] Jedamzik, K. Consistency of Primordial Black Hole Dark Matter with LIGO/Virgo Merger Rates. Phys. Rev. Lett. 126, 051302 (2021). [12] Escrivà, A., Bagui, E. & Clesse, S. Simulations of PBH formation at the QCD epoch and comparison with the GWTC-3 catalog. J. Cosmology Astropart. Phys 2023, 004 (2023). [13] Udalski, A., Szymański, M. K. & Szymański, G. OGLE-IV: Fourth Phase of the Optical Gravitational Lensing Experiment. Acta Astron. 65, 1–38 (2015). [14] Paczyński, B. Gravitational microlensing by the galactic halo. ApJ 304, 1–5 (1986). [15] Alcock, C. et al. The MACHO Project: Microlensing Results from 5.7 Years of Large Magellanic Cloud Observations. ApJ 542, 281–307 (2000). [16] Tisserand, P. et al. Limits on the Macho content of the Galactic Halo from the EROS-2 Survey of the Magellanic Clouds. A&A 469, 387–404 (2007). [17] Wyrzykowski, L. et al. The OGLE view of microlensing towards the Magellanic Clouds - IV. OGLE-III SMC data and final conclusions on MACHOs. MNRAS 416, 2949–2961 (2011). [18] Blaineau, T. et al. New limits from microlensing on Galactic black holes in the mass range 10 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT < M < 1000 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT. A&A 664, A106 (2022). [19] Udalski, A. The Optical Gravitational Lensing Experiment. Real Time Data Analysis Systems in the OGLE-III Survey. Acta Astron. 53, 291–305 (2003). [20] Mróz, P. et al. Microlensing optical depth and event rate toward the Large Magellanic Cloud based on 20 years of OGLE observations. submitted (2024). [21] Holtzman, J. A., Afonso, C. & Dolphin, A. The Local Group Stellar Populations Archive from the Hubble Space Telescope WFPC2. ApJS 166, 534–548 (2006). [22] Mróz, P. et al. No large population of unbound or wide-orbit Jupiter-mass planets. Nature 548, 183–186 (2017). [23] Cautun, M. et al. The milky way total mass profile as inferred from Gaia DR2. MNRAS 494, 4291–4313 (2020). [24] Han, C. & Gould, A. Stellar Contribution to the Galactic Bulge Microlensing Optical Depth. ApJ 592, 172–175 (2003). [25] Niikura, H. et al. Microlensing constraints on primordial black holes with Subaru/HSC Andromeda observations. Nature Astronomy 3, 524–534 (2019). [26] Sahu, K. C. Stars within the Large Magellanic Cloud as potential lenses for observed microlensing events. Nature 370, 275–276 (1994). [27] Erkal, D. et al. The total mass of the Large Magellanic Cloud from its perturbation on the Orphan stream. MNRAS 487, 2685–2700 (2019). [28] Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. A&A 678, A208 (2023). [29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. A distance to the Large Magellanic Cloud that is precise to one per cent. Nature 567, 200–203 (2019). [42] Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. An H I Aperture Synthesis Mosaic of the Large Magellanic Cloud. ApJ 503, 674–688 (1998). [44] Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. The dark matter profile of the Milky Way inferred from its circular velocity curve. MNRAS 528, 693–710 (2024). [45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021). Carr, B., Clesse, S., García-Bellido, J. & Kühnel, F. Cosmic conundra explained by thermal history and primordial black holes. Phys. Dark Universe 31, 100755 (2021). [11] Jedamzik, K. Consistency of Primordial Black Hole Dark Matter with LIGO/Virgo Merger Rates. Phys. Rev. Lett. 126, 051302 (2021). [12] Escrivà, A., Bagui, E. & Clesse, S. Simulations of PBH formation at the QCD epoch and comparison with the GWTC-3 catalog. J. Cosmology Astropart. Phys 2023, 004 (2023). [13] Udalski, A., Szymański, M. K. & Szymański, G. OGLE-IV: Fourth Phase of the Optical Gravitational Lensing Experiment. Acta Astron. 65, 1–38 (2015). [14] Paczyński, B. Gravitational microlensing by the galactic halo. ApJ 304, 1–5 (1986). [15] Alcock, C. et al. The MACHO Project: Microlensing Results from 5.7 Years of Large Magellanic Cloud Observations. ApJ 542, 281–307 (2000). [16] Tisserand, P. et al. Limits on the Macho content of the Galactic Halo from the EROS-2 Survey of the Magellanic Clouds. A&A 469, 387–404 (2007). [17] Wyrzykowski, L. et al. The OGLE view of microlensing towards the Magellanic Clouds - IV. OGLE-III SMC data and final conclusions on MACHOs. MNRAS 416, 2949–2961 (2011). [18] Blaineau, T. et al. New limits from microlensing on Galactic black holes in the mass range 10 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT < M < 1000 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT. A&A 664, A106 (2022). [19] Udalski, A. The Optical Gravitational Lensing Experiment. Real Time Data Analysis Systems in the OGLE-III Survey. Acta Astron. 53, 291–305 (2003). [20] Mróz, P. et al. Microlensing optical depth and event rate toward the Large Magellanic Cloud based on 20 years of OGLE observations. submitted (2024). [21] Holtzman, J. A., Afonso, C. & Dolphin, A. The Local Group Stellar Populations Archive from the Hubble Space Telescope WFPC2. ApJS 166, 534–548 (2006). [22] Mróz, P. et al. No large population of unbound or wide-orbit Jupiter-mass planets. Nature 548, 183–186 (2017). [23] Cautun, M. et al. The milky way total mass profile as inferred from Gaia DR2. MNRAS 494, 4291–4313 (2020). [24] Han, C. & Gould, A. Stellar Contribution to the Galactic Bulge Microlensing Optical Depth. ApJ 592, 172–175 (2003). [25] Niikura, H. et al. Microlensing constraints on primordial black holes with Subaru/HSC Andromeda observations. Nature Astronomy 3, 524–534 (2019). [26] Sahu, K. C. Stars within the Large Magellanic Cloud as potential lenses for observed microlensing events. Nature 370, 275–276 (1994). [27] Erkal, D. et al. The total mass of the Large Magellanic Cloud from its perturbation on the Orphan stream. MNRAS 487, 2685–2700 (2019). [28] Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. A&A 678, A208 (2023). [29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. A distance to the Large Magellanic Cloud that is precise to one per cent. Nature 567, 200–203 (2019). [42] Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. An H I Aperture Synthesis Mosaic of the Large Magellanic Cloud. ApJ 503, 674–688 (1998). [44] Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. The dark matter profile of the Milky Way inferred from its circular velocity curve. MNRAS 528, 693–710 (2024). [45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021). Jedamzik, K. Consistency of Primordial Black Hole Dark Matter with LIGO/Virgo Merger Rates. Phys. Rev. Lett. 126, 051302 (2021). [12] Escrivà, A., Bagui, E. & Clesse, S. Simulations of PBH formation at the QCD epoch and comparison with the GWTC-3 catalog. J. Cosmology Astropart. Phys 2023, 004 (2023). [13] Udalski, A., Szymański, M. K. & Szymański, G. OGLE-IV: Fourth Phase of the Optical Gravitational Lensing Experiment. Acta Astron. 65, 1–38 (2015). [14] Paczyński, B. Gravitational microlensing by the galactic halo. ApJ 304, 1–5 (1986). [15] Alcock, C. et al. The MACHO Project: Microlensing Results from 5.7 Years of Large Magellanic Cloud Observations. ApJ 542, 281–307 (2000). [16] Tisserand, P. et al. Limits on the Macho content of the Galactic Halo from the EROS-2 Survey of the Magellanic Clouds. A&A 469, 387–404 (2007). [17] Wyrzykowski, L. et al. The OGLE view of microlensing towards the Magellanic Clouds - IV. OGLE-III SMC data and final conclusions on MACHOs. MNRAS 416, 2949–2961 (2011). [18] Blaineau, T. et al. New limits from microlensing on Galactic black holes in the mass range 10 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT < M < 1000 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT. A&A 664, A106 (2022). [19] Udalski, A. The Optical Gravitational Lensing Experiment. Real Time Data Analysis Systems in the OGLE-III Survey. Acta Astron. 53, 291–305 (2003). [20] Mróz, P. et al. Microlensing optical depth and event rate toward the Large Magellanic Cloud based on 20 years of OGLE observations. submitted (2024). [21] Holtzman, J. A., Afonso, C. & Dolphin, A. The Local Group Stellar Populations Archive from the Hubble Space Telescope WFPC2. ApJS 166, 534–548 (2006). [22] Mróz, P. et al. No large population of unbound or wide-orbit Jupiter-mass planets. Nature 548, 183–186 (2017). [23] Cautun, M. et al. The milky way total mass profile as inferred from Gaia DR2. MNRAS 494, 4291–4313 (2020). [24] Han, C. & Gould, A. Stellar Contribution to the Galactic Bulge Microlensing Optical Depth. ApJ 592, 172–175 (2003). [25] Niikura, H. et al. Microlensing constraints on primordial black holes with Subaru/HSC Andromeda observations. Nature Astronomy 3, 524–534 (2019). [26] Sahu, K. C. Stars within the Large Magellanic Cloud as potential lenses for observed microlensing events. Nature 370, 275–276 (1994). [27] Erkal, D. et al. The total mass of the Large Magellanic Cloud from its perturbation on the Orphan stream. MNRAS 487, 2685–2700 (2019). [28] Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. A&A 678, A208 (2023). [29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. 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The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. A distance to the Large Magellanic Cloud that is precise to one per cent. Nature 567, 200–203 (2019). [42] Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. An H I Aperture Synthesis Mosaic of the Large Magellanic Cloud. ApJ 503, 674–688 (1998). [44] Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. The dark matter profile of the Milky Way inferred from its circular velocity curve. MNRAS 528, 693–710 (2024). [45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021). Udalski, A., Szymański, M. K. & Szymański, G. OGLE-IV: Fourth Phase of the Optical Gravitational Lensing Experiment. Acta Astron. 65, 1–38 (2015). [14] Paczyński, B. Gravitational microlensing by the galactic halo. ApJ 304, 1–5 (1986). [15] Alcock, C. et al. The MACHO Project: Microlensing Results from 5.7 Years of Large Magellanic Cloud Observations. ApJ 542, 281–307 (2000). [16] Tisserand, P. et al. Limits on the Macho content of the Galactic Halo from the EROS-2 Survey of the Magellanic Clouds. A&A 469, 387–404 (2007). [17] Wyrzykowski, L. et al. The OGLE view of microlensing towards the Magellanic Clouds - IV. OGLE-III SMC data and final conclusions on MACHOs. MNRAS 416, 2949–2961 (2011). [18] Blaineau, T. et al. New limits from microlensing on Galactic black holes in the mass range 10 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT < M < 1000 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT. A&A 664, A106 (2022). [19] Udalski, A. The Optical Gravitational Lensing Experiment. Real Time Data Analysis Systems in the OGLE-III Survey. Acta Astron. 53, 291–305 (2003). [20] Mróz, P. et al. Microlensing optical depth and event rate toward the Large Magellanic Cloud based on 20 years of OGLE observations. submitted (2024). [21] Holtzman, J. A., Afonso, C. & Dolphin, A. The Local Group Stellar Populations Archive from the Hubble Space Telescope WFPC2. ApJS 166, 534–548 (2006). [22] Mróz, P. et al. No large population of unbound or wide-orbit Jupiter-mass planets. Nature 548, 183–186 (2017). [23] Cautun, M. et al. The milky way total mass profile as inferred from Gaia DR2. MNRAS 494, 4291–4313 (2020). [24] Han, C. & Gould, A. Stellar Contribution to the Galactic Bulge Microlensing Optical Depth. ApJ 592, 172–175 (2003). [25] Niikura, H. et al. Microlensing constraints on primordial black holes with Subaru/HSC Andromeda observations. Nature Astronomy 3, 524–534 (2019). [26] Sahu, K. C. Stars within the Large Magellanic Cloud as potential lenses for observed microlensing events. Nature 370, 275–276 (1994). [27] Erkal, D. et al. The total mass of the Large Magellanic Cloud from its perturbation on the Orphan stream. MNRAS 487, 2685–2700 (2019). [28] Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. A&A 678, A208 (2023). [29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. 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Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021). Paczyński, B. Gravitational microlensing by the galactic halo. ApJ 304, 1–5 (1986). [15] Alcock, C. et al. The MACHO Project: Microlensing Results from 5.7 Years of Large Magellanic Cloud Observations. ApJ 542, 281–307 (2000). [16] Tisserand, P. et al. Limits on the Macho content of the Galactic Halo from the EROS-2 Survey of the Magellanic Clouds. A&A 469, 387–404 (2007). [17] Wyrzykowski, L. et al. The OGLE view of microlensing towards the Magellanic Clouds - IV. OGLE-III SMC data and final conclusions on MACHOs. MNRAS 416, 2949–2961 (2011). [18] Blaineau, T. et al. New limits from microlensing on Galactic black holes in the mass range 10 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT < M < 1000 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT. A&A 664, A106 (2022). [19] Udalski, A. The Optical Gravitational Lensing Experiment. Real Time Data Analysis Systems in the OGLE-III Survey. Acta Astron. 53, 291–305 (2003). [20] Mróz, P. et al. Microlensing optical depth and event rate toward the Large Magellanic Cloud based on 20 years of OGLE observations. submitted (2024). [21] Holtzman, J. A., Afonso, C. & Dolphin, A. The Local Group Stellar Populations Archive from the Hubble Space Telescope WFPC2. ApJS 166, 534–548 (2006). [22] Mróz, P. et al. No large population of unbound or wide-orbit Jupiter-mass planets. Nature 548, 183–186 (2017). [23] Cautun, M. et al. The milky way total mass profile as inferred from Gaia DR2. MNRAS 494, 4291–4313 (2020). [24] Han, C. & Gould, A. Stellar Contribution to the Galactic Bulge Microlensing Optical Depth. ApJ 592, 172–175 (2003). [25] Niikura, H. et al. Microlensing constraints on primordial black holes with Subaru/HSC Andromeda observations. Nature Astronomy 3, 524–534 (2019). [26] Sahu, K. C. Stars within the Large Magellanic Cloud as potential lenses for observed microlensing events. Nature 370, 275–276 (1994). [27] Erkal, D. et al. The total mass of the Large Magellanic Cloud from its perturbation on the Orphan stream. MNRAS 487, 2685–2700 (2019). [28] Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. A&A 678, A208 (2023). [29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. 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ApJ 542, 281–307 (2000). [16] Tisserand, P. et al. Limits on the Macho content of the Galactic Halo from the EROS-2 Survey of the Magellanic Clouds. A&A 469, 387–404 (2007). [17] Wyrzykowski, L. et al. The OGLE view of microlensing towards the Magellanic Clouds - IV. OGLE-III SMC data and final conclusions on MACHOs. MNRAS 416, 2949–2961 (2011). [18] Blaineau, T. et al. New limits from microlensing on Galactic black holes in the mass range 10 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT < M < 1000 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT. A&A 664, A106 (2022). [19] Udalski, A. The Optical Gravitational Lensing Experiment. Real Time Data Analysis Systems in the OGLE-III Survey. Acta Astron. 53, 291–305 (2003). [20] Mróz, P. et al. Microlensing optical depth and event rate toward the Large Magellanic Cloud based on 20 years of OGLE observations. submitted (2024). [21] Holtzman, J. A., Afonso, C. & Dolphin, A. The Local Group Stellar Populations Archive from the Hubble Space Telescope WFPC2. ApJS 166, 534–548 (2006). [22] Mróz, P. et al. No large population of unbound or wide-orbit Jupiter-mass planets. Nature 548, 183–186 (2017). [23] Cautun, M. et al. The milky way total mass profile as inferred from Gaia DR2. MNRAS 494, 4291–4313 (2020). [24] Han, C. & Gould, A. Stellar Contribution to the Galactic Bulge Microlensing Optical Depth. ApJ 592, 172–175 (2003). [25] Niikura, H. et al. Microlensing constraints on primordial black holes with Subaru/HSC Andromeda observations. Nature Astronomy 3, 524–534 (2019). [26] Sahu, K. C. Stars within the Large Magellanic Cloud as potential lenses for observed microlensing events. Nature 370, 275–276 (1994). [27] Erkal, D. et al. The total mass of the Large Magellanic Cloud from its perturbation on the Orphan stream. MNRAS 487, 2685–2700 (2019). [28] Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. A&A 678, A208 (2023). [29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. A distance to the Large Magellanic Cloud that is precise to one per cent. Nature 567, 200–203 (2019). [42] Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. An H I Aperture Synthesis Mosaic of the Large Magellanic Cloud. ApJ 503, 674–688 (1998). [44] Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. The dark matter profile of the Milky Way inferred from its circular velocity curve. MNRAS 528, 693–710 (2024). [45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021). Tisserand, P. et al. Limits on the Macho content of the Galactic Halo from the EROS-2 Survey of the Magellanic Clouds. A&A 469, 387–404 (2007). [17] Wyrzykowski, L. et al. The OGLE view of microlensing towards the Magellanic Clouds - IV. OGLE-III SMC data and final conclusions on MACHOs. MNRAS 416, 2949–2961 (2011). [18] Blaineau, T. et al. New limits from microlensing on Galactic black holes in the mass range 10 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT < M < 1000 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT. A&A 664, A106 (2022). [19] Udalski, A. The Optical Gravitational Lensing Experiment. Real Time Data Analysis Systems in the OGLE-III Survey. Acta Astron. 53, 291–305 (2003). [20] Mróz, P. et al. Microlensing optical depth and event rate toward the Large Magellanic Cloud based on 20 years of OGLE observations. submitted (2024). [21] Holtzman, J. A., Afonso, C. & Dolphin, A. The Local Group Stellar Populations Archive from the Hubble Space Telescope WFPC2. ApJS 166, 534–548 (2006). [22] Mróz, P. et al. No large population of unbound or wide-orbit Jupiter-mass planets. Nature 548, 183–186 (2017). [23] Cautun, M. et al. The milky way total mass profile as inferred from Gaia DR2. MNRAS 494, 4291–4313 (2020). [24] Han, C. & Gould, A. 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The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. 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[36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. A distance to the Large Magellanic Cloud that is precise to one per cent. Nature 567, 200–203 (2019). [42] Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. 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[9] Clesse, S. & García-Bellido, J. The clustering of massive Primordial Black Holes as Dark Matter: Measuring their mass distribution with advanced LIGO. Phys. Dark Universe 15, 142–147 (2017). [10] Carr, B., Clesse, S., García-Bellido, J. & Kühnel, F. Cosmic conundra explained by thermal history and primordial black holes. Phys. Dark Universe 31, 100755 (2021). [11] Jedamzik, K. Consistency of Primordial Black Hole Dark Matter with LIGO/Virgo Merger Rates. Phys. Rev. Lett. 126, 051302 (2021). [12] Escrivà, A., Bagui, E. & Clesse, S. Simulations of PBH formation at the QCD epoch and comparison with the GWTC-3 catalog. J. Cosmology Astropart. Phys 2023, 004 (2023). [13] Udalski, A., Szymański, M. K. & Szymański, G. OGLE-IV: Fourth Phase of the Optical Gravitational Lensing Experiment. Acta Astron. 65, 1–38 (2015). [14] Paczyński, B. Gravitational microlensing by the galactic halo. ApJ 304, 1–5 (1986). [15] Alcock, C. et al. 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The total mass of the Large Magellanic Cloud from its perturbation on the Orphan stream. MNRAS 487, 2685–2700 (2019). [28] Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. A&A 678, A208 (2023). [29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. 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[9] Clesse, S. & García-Bellido, J. The clustering of massive Primordial Black Holes as Dark Matter: Measuring their mass distribution with advanced LIGO. Phys. Dark Universe 15, 142–147 (2017). [10] Carr, B., Clesse, S., García-Bellido, J. & Kühnel, F. Cosmic conundra explained by thermal history and primordial black holes. Phys. Dark Universe 31, 100755 (2021). [11] Jedamzik, K. Consistency of Primordial Black Hole Dark Matter with LIGO/Virgo Merger Rates. Phys. Rev. Lett. 126, 051302 (2021). [12] Escrivà, A., Bagui, E. & Clesse, S. Simulations of PBH formation at the QCD epoch and comparison with the GWTC-3 catalog. J. Cosmology Astropart. Phys 2023, 004 (2023). [13] Udalski, A., Szymański, M. K. & Szymański, G. OGLE-IV: Fourth Phase of the Optical Gravitational Lensing Experiment. Acta Astron. 65, 1–38 (2015). [14] Paczyński, B. Gravitational microlensing by the galactic halo. ApJ 304, 1–5 (1986). [15] Alcock, C. et al. The MACHO Project: Microlensing Results from 5.7 Years of Large Magellanic Cloud Observations. ApJ 542, 281–307 (2000). [16] Tisserand, P. et al. Limits on the Macho content of the Galactic Halo from the EROS-2 Survey of the Magellanic Clouds. A&A 469, 387–404 (2007). [17] Wyrzykowski, L. et al. The OGLE view of microlensing towards the Magellanic Clouds - IV. OGLE-III SMC data and final conclusions on MACHOs. MNRAS 416, 2949–2961 (2011). [18] Blaineau, T. et al. New limits from microlensing on Galactic black holes in the mass range 10 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT < M < 1000 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT. A&A 664, A106 (2022). [19] Udalski, A. The Optical Gravitational Lensing Experiment. Real Time Data Analysis Systems in the OGLE-III Survey. Acta Astron. 53, 291–305 (2003). [20] Mróz, P. et al. Microlensing optical depth and event rate toward the Large Magellanic Cloud based on 20 years of OGLE observations. submitted (2024). [21] Holtzman, J. A., Afonso, C. & Dolphin, A. The Local Group Stellar Populations Archive from the Hubble Space Telescope WFPC2. ApJS 166, 534–548 (2006). [22] Mróz, P. et al. No large population of unbound or wide-orbit Jupiter-mass planets. Nature 548, 183–186 (2017). [23] Cautun, M. et al. The milky way total mass profile as inferred from Gaia DR2. MNRAS 494, 4291–4313 (2020). [24] Han, C. & Gould, A. Stellar Contribution to the Galactic Bulge Microlensing Optical Depth. ApJ 592, 172–175 (2003). [25] Niikura, H. et al. Microlensing constraints on primordial black holes with Subaru/HSC Andromeda observations. Nature Astronomy 3, 524–534 (2019). [26] Sahu, K. C. Stars within the Large Magellanic Cloud as potential lenses for observed microlensing events. Nature 370, 275–276 (1994). [27] Erkal, D. et al. The total mass of the Large Magellanic Cloud from its perturbation on the Orphan stream. MNRAS 487, 2685–2700 (2019). [28] Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. A&A 678, A208 (2023). [29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. A distance to the Large Magellanic Cloud that is precise to one per cent. Nature 567, 200–203 (2019). [42] Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. An H I Aperture Synthesis Mosaic of the Large Magellanic Cloud. ApJ 503, 674–688 (1998). [44] Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. The dark matter profile of the Milky Way inferred from its circular velocity curve. MNRAS 528, 693–710 (2024). [45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021). Sasaki, M., Suyama, T., Tanaka, T. & Yokoyama, S. Primordial Black Hole Scenario for the Gravitational-Wave Event GW150914. Phys. Rev. Lett. 117, 061101 (2016). [9] Clesse, S. & García-Bellido, J. The clustering of massive Primordial Black Holes as Dark Matter: Measuring their mass distribution with advanced LIGO. Phys. Dark Universe 15, 142–147 (2017). [10] Carr, B., Clesse, S., García-Bellido, J. & Kühnel, F. Cosmic conundra explained by thermal history and primordial black holes. Phys. Dark Universe 31, 100755 (2021). [11] Jedamzik, K. Consistency of Primordial Black Hole Dark Matter with LIGO/Virgo Merger Rates. Phys. Rev. Lett. 126, 051302 (2021). [12] Escrivà, A., Bagui, E. & Clesse, S. Simulations of PBH formation at the QCD epoch and comparison with the GWTC-3 catalog. J. Cosmology Astropart. Phys 2023, 004 (2023). [13] Udalski, A., Szymański, M. K. & Szymański, G. OGLE-IV: Fourth Phase of the Optical Gravitational Lensing Experiment. Acta Astron. 65, 1–38 (2015). [14] Paczyński, B. Gravitational microlensing by the galactic halo. ApJ 304, 1–5 (1986). [15] Alcock, C. et al. The MACHO Project: Microlensing Results from 5.7 Years of Large Magellanic Cloud Observations. ApJ 542, 281–307 (2000). [16] Tisserand, P. et al. Limits on the Macho content of the Galactic Halo from the EROS-2 Survey of the Magellanic Clouds. A&A 469, 387–404 (2007). [17] Wyrzykowski, L. et al. The OGLE view of microlensing towards the Magellanic Clouds - IV. OGLE-III SMC data and final conclusions on MACHOs. MNRAS 416, 2949–2961 (2011). [18] Blaineau, T. et al. New limits from microlensing on Galactic black holes in the mass range 10 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT < M < 1000 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT. A&A 664, A106 (2022). [19] Udalski, A. The Optical Gravitational Lensing Experiment. Real Time Data Analysis Systems in the OGLE-III Survey. Acta Astron. 53, 291–305 (2003). [20] Mróz, P. et al. Microlensing optical depth and event rate toward the Large Magellanic Cloud based on 20 years of OGLE observations. submitted (2024). [21] Holtzman, J. A., Afonso, C. & Dolphin, A. The Local Group Stellar Populations Archive from the Hubble Space Telescope WFPC2. ApJS 166, 534–548 (2006). [22] Mróz, P. et al. No large population of unbound or wide-orbit Jupiter-mass planets. Nature 548, 183–186 (2017). [23] Cautun, M. et al. The milky way total mass profile as inferred from Gaia DR2. MNRAS 494, 4291–4313 (2020). [24] Han, C. & Gould, A. Stellar Contribution to the Galactic Bulge Microlensing Optical Depth. ApJ 592, 172–175 (2003). [25] Niikura, H. et al. Microlensing constraints on primordial black holes with Subaru/HSC Andromeda observations. Nature Astronomy 3, 524–534 (2019). [26] Sahu, K. C. Stars within the Large Magellanic Cloud as potential lenses for observed microlensing events. Nature 370, 275–276 (1994). [27] Erkal, D. et al. The total mass of the Large Magellanic Cloud from its perturbation on the Orphan stream. MNRAS 487, 2685–2700 (2019). [28] Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. A&A 678, A208 (2023). [29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. A distance to the Large Magellanic Cloud that is precise to one per cent. Nature 567, 200–203 (2019). [42] Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. An H I Aperture Synthesis Mosaic of the Large Magellanic Cloud. ApJ 503, 674–688 (1998). [44] Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. The dark matter profile of the Milky Way inferred from its circular velocity curve. MNRAS 528, 693–710 (2024). [45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021). Clesse, S. & García-Bellido, J. The clustering of massive Primordial Black Holes as Dark Matter: Measuring their mass distribution with advanced LIGO. Phys. Dark Universe 15, 142–147 (2017). [10] Carr, B., Clesse, S., García-Bellido, J. & Kühnel, F. Cosmic conundra explained by thermal history and primordial black holes. Phys. Dark Universe 31, 100755 (2021). [11] Jedamzik, K. Consistency of Primordial Black Hole Dark Matter with LIGO/Virgo Merger Rates. Phys. Rev. Lett. 126, 051302 (2021). [12] Escrivà, A., Bagui, E. & Clesse, S. Simulations of PBH formation at the QCD epoch and comparison with the GWTC-3 catalog. J. Cosmology Astropart. Phys 2023, 004 (2023). [13] Udalski, A., Szymański, M. K. & Szymański, G. OGLE-IV: Fourth Phase of the Optical Gravitational Lensing Experiment. Acta Astron. 65, 1–38 (2015). [14] Paczyński, B. Gravitational microlensing by the galactic halo. ApJ 304, 1–5 (1986). [15] Alcock, C. et al. The MACHO Project: Microlensing Results from 5.7 Years of Large Magellanic Cloud Observations. ApJ 542, 281–307 (2000). [16] Tisserand, P. et al. Limits on the Macho content of the Galactic Halo from the EROS-2 Survey of the Magellanic Clouds. A&A 469, 387–404 (2007). [17] Wyrzykowski, L. et al. The OGLE view of microlensing towards the Magellanic Clouds - IV. OGLE-III SMC data and final conclusions on MACHOs. MNRAS 416, 2949–2961 (2011). [18] Blaineau, T. et al. New limits from microlensing on Galactic black holes in the mass range 10 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT < M < 1000 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT. A&A 664, A106 (2022). [19] Udalski, A. The Optical Gravitational Lensing Experiment. Real Time Data Analysis Systems in the OGLE-III Survey. Acta Astron. 53, 291–305 (2003). [20] Mróz, P. et al. Microlensing optical depth and event rate toward the Large Magellanic Cloud based on 20 years of OGLE observations. submitted (2024). [21] Holtzman, J. A., Afonso, C. & Dolphin, A. The Local Group Stellar Populations Archive from the Hubble Space Telescope WFPC2. ApJS 166, 534–548 (2006). [22] Mróz, P. et al. No large population of unbound or wide-orbit Jupiter-mass planets. Nature 548, 183–186 (2017). [23] Cautun, M. et al. The milky way total mass profile as inferred from Gaia DR2. MNRAS 494, 4291–4313 (2020). [24] Han, C. & Gould, A. Stellar Contribution to the Galactic Bulge Microlensing Optical Depth. ApJ 592, 172–175 (2003). [25] Niikura, H. et al. Microlensing constraints on primordial black holes with Subaru/HSC Andromeda observations. Nature Astronomy 3, 524–534 (2019). [26] Sahu, K. C. Stars within the Large Magellanic Cloud as potential lenses for observed microlensing events. Nature 370, 275–276 (1994). [27] Erkal, D. et al. The total mass of the Large Magellanic Cloud from its perturbation on the Orphan stream. MNRAS 487, 2685–2700 (2019). [28] Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. A&A 678, A208 (2023). [29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. A distance to the Large Magellanic Cloud that is precise to one per cent. Nature 567, 200–203 (2019). [42] Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. An H I Aperture Synthesis Mosaic of the Large Magellanic Cloud. ApJ 503, 674–688 (1998). [44] Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. The dark matter profile of the Milky Way inferred from its circular velocity curve. MNRAS 528, 693–710 (2024). [45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021). Carr, B., Clesse, S., García-Bellido, J. & Kühnel, F. Cosmic conundra explained by thermal history and primordial black holes. Phys. Dark Universe 31, 100755 (2021). [11] Jedamzik, K. Consistency of Primordial Black Hole Dark Matter with LIGO/Virgo Merger Rates. Phys. Rev. Lett. 126, 051302 (2021). [12] Escrivà, A., Bagui, E. & Clesse, S. Simulations of PBH formation at the QCD epoch and comparison with the GWTC-3 catalog. J. Cosmology Astropart. Phys 2023, 004 (2023). [13] Udalski, A., Szymański, M. K. & Szymański, G. OGLE-IV: Fourth Phase of the Optical Gravitational Lensing Experiment. Acta Astron. 65, 1–38 (2015). [14] Paczyński, B. Gravitational microlensing by the galactic halo. ApJ 304, 1–5 (1986). [15] Alcock, C. et al. The MACHO Project: Microlensing Results from 5.7 Years of Large Magellanic Cloud Observations. ApJ 542, 281–307 (2000). [16] Tisserand, P. et al. Limits on the Macho content of the Galactic Halo from the EROS-2 Survey of the Magellanic Clouds. A&A 469, 387–404 (2007). [17] Wyrzykowski, L. et al. The OGLE view of microlensing towards the Magellanic Clouds - IV. OGLE-III SMC data and final conclusions on MACHOs. MNRAS 416, 2949–2961 (2011). [18] Blaineau, T. et al. New limits from microlensing on Galactic black holes in the mass range 10 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT < M < 1000 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT. A&A 664, A106 (2022). [19] Udalski, A. The Optical Gravitational Lensing Experiment. Real Time Data Analysis Systems in the OGLE-III Survey. Acta Astron. 53, 291–305 (2003). [20] Mróz, P. et al. Microlensing optical depth and event rate toward the Large Magellanic Cloud based on 20 years of OGLE observations. submitted (2024). [21] Holtzman, J. A., Afonso, C. & Dolphin, A. The Local Group Stellar Populations Archive from the Hubble Space Telescope WFPC2. ApJS 166, 534–548 (2006). [22] Mróz, P. et al. No large population of unbound or wide-orbit Jupiter-mass planets. Nature 548, 183–186 (2017). [23] Cautun, M. et al. The milky way total mass profile as inferred from Gaia DR2. MNRAS 494, 4291–4313 (2020). [24] Han, C. & Gould, A. Stellar Contribution to the Galactic Bulge Microlensing Optical Depth. ApJ 592, 172–175 (2003). [25] Niikura, H. et al. Microlensing constraints on primordial black holes with Subaru/HSC Andromeda observations. Nature Astronomy 3, 524–534 (2019). [26] Sahu, K. C. Stars within the Large Magellanic Cloud as potential lenses for observed microlensing events. Nature 370, 275–276 (1994). [27] Erkal, D. et al. The total mass of the Large Magellanic Cloud from its perturbation on the Orphan stream. MNRAS 487, 2685–2700 (2019). [28] Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. A&A 678, A208 (2023). [29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. A distance to the Large Magellanic Cloud that is precise to one per cent. Nature 567, 200–203 (2019). [42] Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. An H I Aperture Synthesis Mosaic of the Large Magellanic Cloud. ApJ 503, 674–688 (1998). [44] Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. The dark matter profile of the Milky Way inferred from its circular velocity curve. MNRAS 528, 693–710 (2024). [45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021). Jedamzik, K. Consistency of Primordial Black Hole Dark Matter with LIGO/Virgo Merger Rates. Phys. Rev. Lett. 126, 051302 (2021). [12] Escrivà, A., Bagui, E. & Clesse, S. Simulations of PBH formation at the QCD epoch and comparison with the GWTC-3 catalog. J. Cosmology Astropart. Phys 2023, 004 (2023). [13] Udalski, A., Szymański, M. K. & Szymański, G. OGLE-IV: Fourth Phase of the Optical Gravitational Lensing Experiment. Acta Astron. 65, 1–38 (2015). [14] Paczyński, B. Gravitational microlensing by the galactic halo. ApJ 304, 1–5 (1986). [15] Alcock, C. et al. The MACHO Project: Microlensing Results from 5.7 Years of Large Magellanic Cloud Observations. ApJ 542, 281–307 (2000). [16] Tisserand, P. et al. Limits on the Macho content of the Galactic Halo from the EROS-2 Survey of the Magellanic Clouds. A&A 469, 387–404 (2007). [17] Wyrzykowski, L. et al. The OGLE view of microlensing towards the Magellanic Clouds - IV. OGLE-III SMC data and final conclusions on MACHOs. MNRAS 416, 2949–2961 (2011). [18] Blaineau, T. et al. New limits from microlensing on Galactic black holes in the mass range 10 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT < M < 1000 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT. A&A 664, A106 (2022). [19] Udalski, A. The Optical Gravitational Lensing Experiment. Real Time Data Analysis Systems in the OGLE-III Survey. Acta Astron. 53, 291–305 (2003). [20] Mróz, P. et al. Microlensing optical depth and event rate toward the Large Magellanic Cloud based on 20 years of OGLE observations. submitted (2024). [21] Holtzman, J. A., Afonso, C. & Dolphin, A. The Local Group Stellar Populations Archive from the Hubble Space Telescope WFPC2. ApJS 166, 534–548 (2006). [22] Mróz, P. et al. No large population of unbound or wide-orbit Jupiter-mass planets. Nature 548, 183–186 (2017). [23] Cautun, M. et al. The milky way total mass profile as inferred from Gaia DR2. MNRAS 494, 4291–4313 (2020). [24] Han, C. & Gould, A. Stellar Contribution to the Galactic Bulge Microlensing Optical Depth. ApJ 592, 172–175 (2003). [25] Niikura, H. et al. Microlensing constraints on primordial black holes with Subaru/HSC Andromeda observations. Nature Astronomy 3, 524–534 (2019). [26] Sahu, K. C. Stars within the Large Magellanic Cloud as potential lenses for observed microlensing events. Nature 370, 275–276 (1994). [27] Erkal, D. et al. The total mass of the Large Magellanic Cloud from its perturbation on the Orphan stream. MNRAS 487, 2685–2700 (2019). [28] Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. A&A 678, A208 (2023). [29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. A distance to the Large Magellanic Cloud that is precise to one per cent. Nature 567, 200–203 (2019). [42] Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. An H I Aperture Synthesis Mosaic of the Large Magellanic Cloud. ApJ 503, 674–688 (1998). [44] Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. The dark matter profile of the Milky Way inferred from its circular velocity curve. MNRAS 528, 693–710 (2024). [45] Gaia Collaboration et al. Gaia Data Release 2. 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The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. A distance to the Large Magellanic Cloud that is precise to one per cent. Nature 567, 200–203 (2019). [42] Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. An H I Aperture Synthesis Mosaic of the Large Magellanic Cloud. ApJ 503, 674–688 (1998). [44] Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. The dark matter profile of the Milky Way inferred from its circular velocity curve. MNRAS 528, 693–710 (2024). [45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021). Udalski, A., Szymański, M. K. & Szymański, G. OGLE-IV: Fourth Phase of the Optical Gravitational Lensing Experiment. Acta Astron. 65, 1–38 (2015). [14] Paczyński, B. Gravitational microlensing by the galactic halo. ApJ 304, 1–5 (1986). [15] Alcock, C. et al. The MACHO Project: Microlensing Results from 5.7 Years of Large Magellanic Cloud Observations. ApJ 542, 281–307 (2000). [16] Tisserand, P. et al. Limits on the Macho content of the Galactic Halo from the EROS-2 Survey of the Magellanic Clouds. A&A 469, 387–404 (2007). [17] Wyrzykowski, L. et al. The OGLE view of microlensing towards the Magellanic Clouds - IV. OGLE-III SMC data and final conclusions on MACHOs. MNRAS 416, 2949–2961 (2011). [18] Blaineau, T. et al. New limits from microlensing on Galactic black holes in the mass range 10 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT < M < 1000 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT. A&A 664, A106 (2022). [19] Udalski, A. The Optical Gravitational Lensing Experiment. Real Time Data Analysis Systems in the OGLE-III Survey. Acta Astron. 53, 291–305 (2003). [20] Mróz, P. et al. Microlensing optical depth and event rate toward the Large Magellanic Cloud based on 20 years of OGLE observations. submitted (2024). [21] Holtzman, J. A., Afonso, C. & Dolphin, A. The Local Group Stellar Populations Archive from the Hubble Space Telescope WFPC2. ApJS 166, 534–548 (2006). [22] Mróz, P. et al. No large population of unbound or wide-orbit Jupiter-mass planets. Nature 548, 183–186 (2017). [23] Cautun, M. et al. The milky way total mass profile as inferred from Gaia DR2. MNRAS 494, 4291–4313 (2020). [24] Han, C. & Gould, A. Stellar Contribution to the Galactic Bulge Microlensing Optical Depth. ApJ 592, 172–175 (2003). [25] Niikura, H. et al. Microlensing constraints on primordial black holes with Subaru/HSC Andromeda observations. Nature Astronomy 3, 524–534 (2019). [26] Sahu, K. C. Stars within the Large Magellanic Cloud as potential lenses for observed microlensing events. Nature 370, 275–276 (1994). [27] Erkal, D. et al. The total mass of the Large Magellanic Cloud from its perturbation on the Orphan stream. MNRAS 487, 2685–2700 (2019). [28] Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. A&A 678, A208 (2023). [29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. A distance to the Large Magellanic Cloud that is precise to one per cent. Nature 567, 200–203 (2019). [42] Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. An H I Aperture Synthesis Mosaic of the Large Magellanic Cloud. ApJ 503, 674–688 (1998). [44] Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. The dark matter profile of the Milky Way inferred from its circular velocity curve. MNRAS 528, 693–710 (2024). [45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021). Paczyński, B. Gravitational microlensing by the galactic halo. ApJ 304, 1–5 (1986). [15] Alcock, C. et al. The MACHO Project: Microlensing Results from 5.7 Years of Large Magellanic Cloud Observations. ApJ 542, 281–307 (2000). [16] Tisserand, P. et al. Limits on the Macho content of the Galactic Halo from the EROS-2 Survey of the Magellanic Clouds. A&A 469, 387–404 (2007). [17] Wyrzykowski, L. et al. The OGLE view of microlensing towards the Magellanic Clouds - IV. OGLE-III SMC data and final conclusions on MACHOs. MNRAS 416, 2949–2961 (2011). [18] Blaineau, T. et al. New limits from microlensing on Galactic black holes in the mass range 10 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT < M < 1000 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT. A&A 664, A106 (2022). [19] Udalski, A. The Optical Gravitational Lensing Experiment. Real Time Data Analysis Systems in the OGLE-III Survey. Acta Astron. 53, 291–305 (2003). [20] Mróz, P. et al. Microlensing optical depth and event rate toward the Large Magellanic Cloud based on 20 years of OGLE observations. submitted (2024). [21] Holtzman, J. A., Afonso, C. & Dolphin, A. The Local Group Stellar Populations Archive from the Hubble Space Telescope WFPC2. ApJS 166, 534–548 (2006). [22] Mróz, P. et al. No large population of unbound or wide-orbit Jupiter-mass planets. Nature 548, 183–186 (2017). [23] Cautun, M. et al. The milky way total mass profile as inferred from Gaia DR2. MNRAS 494, 4291–4313 (2020). [24] Han, C. & Gould, A. Stellar Contribution to the Galactic Bulge Microlensing Optical Depth. ApJ 592, 172–175 (2003). [25] Niikura, H. et al. Microlensing constraints on primordial black holes with Subaru/HSC Andromeda observations. Nature Astronomy 3, 524–534 (2019). [26] Sahu, K. C. Stars within the Large Magellanic Cloud as potential lenses for observed microlensing events. Nature 370, 275–276 (1994). [27] Erkal, D. et al. The total mass of the Large Magellanic Cloud from its perturbation on the Orphan stream. MNRAS 487, 2685–2700 (2019). [28] Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. A&A 678, A208 (2023). [29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. A distance to the Large Magellanic Cloud that is precise to one per cent. Nature 567, 200–203 (2019). [42] Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. An H I Aperture Synthesis Mosaic of the Large Magellanic Cloud. ApJ 503, 674–688 (1998). [44] Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. The dark matter profile of the Milky Way inferred from its circular velocity curve. MNRAS 528, 693–710 (2024). [45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021). Alcock, C. et al. The MACHO Project: Microlensing Results from 5.7 Years of Large Magellanic Cloud Observations. ApJ 542, 281–307 (2000). [16] Tisserand, P. et al. Limits on the Macho content of the Galactic Halo from the EROS-2 Survey of the Magellanic Clouds. A&A 469, 387–404 (2007). [17] Wyrzykowski, L. et al. The OGLE view of microlensing towards the Magellanic Clouds - IV. OGLE-III SMC data and final conclusions on MACHOs. MNRAS 416, 2949–2961 (2011). [18] Blaineau, T. et al. New limits from microlensing on Galactic black holes in the mass range 10 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT < M < 1000 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT. A&A 664, A106 (2022). [19] Udalski, A. The Optical Gravitational Lensing Experiment. Real Time Data Analysis Systems in the OGLE-III Survey. Acta Astron. 53, 291–305 (2003). [20] Mróz, P. et al. Microlensing optical depth and event rate toward the Large Magellanic Cloud based on 20 years of OGLE observations. submitted (2024). [21] Holtzman, J. A., Afonso, C. & Dolphin, A. The Local Group Stellar Populations Archive from the Hubble Space Telescope WFPC2. ApJS 166, 534–548 (2006). [22] Mróz, P. et al. No large population of unbound or wide-orbit Jupiter-mass planets. Nature 548, 183–186 (2017). [23] Cautun, M. et al. The milky way total mass profile as inferred from Gaia DR2. MNRAS 494, 4291–4313 (2020). [24] Han, C. & Gould, A. Stellar Contribution to the Galactic Bulge Microlensing Optical Depth. ApJ 592, 172–175 (2003). [25] Niikura, H. et al. Microlensing constraints on primordial black holes with Subaru/HSC Andromeda observations. Nature Astronomy 3, 524–534 (2019). [26] Sahu, K. C. Stars within the Large Magellanic Cloud as potential lenses for observed microlensing events. Nature 370, 275–276 (1994). [27] Erkal, D. et al. The total mass of the Large Magellanic Cloud from its perturbation on the Orphan stream. MNRAS 487, 2685–2700 (2019). [28] Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. A&A 678, A208 (2023). [29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. A distance to the Large Magellanic Cloud that is precise to one per cent. Nature 567, 200–203 (2019). [42] Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. An H I Aperture Synthesis Mosaic of the Large Magellanic Cloud. ApJ 503, 674–688 (1998). [44] Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. The dark matter profile of the Milky Way inferred from its circular velocity curve. MNRAS 528, 693–710 (2024). [45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021). Tisserand, P. et al. Limits on the Macho content of the Galactic Halo from the EROS-2 Survey of the Magellanic Clouds. A&A 469, 387–404 (2007). [17] Wyrzykowski, L. et al. The OGLE view of microlensing towards the Magellanic Clouds - IV. OGLE-III SMC data and final conclusions on MACHOs. MNRAS 416, 2949–2961 (2011). [18] Blaineau, T. et al. New limits from microlensing on Galactic black holes in the mass range 10 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT < M < 1000 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT. A&A 664, A106 (2022). [19] Udalski, A. The Optical Gravitational Lensing Experiment. Real Time Data Analysis Systems in the OGLE-III Survey. Acta Astron. 53, 291–305 (2003). [20] Mróz, P. et al. Microlensing optical depth and event rate toward the Large Magellanic Cloud based on 20 years of OGLE observations. submitted (2024). [21] Holtzman, J. A., Afonso, C. & Dolphin, A. The Local Group Stellar Populations Archive from the Hubble Space Telescope WFPC2. ApJS 166, 534–548 (2006). [22] Mróz, P. et al. No large population of unbound or wide-orbit Jupiter-mass planets. Nature 548, 183–186 (2017). [23] Cautun, M. et al. The milky way total mass profile as inferred from Gaia DR2. MNRAS 494, 4291–4313 (2020). [24] Han, C. & Gould, A. Stellar Contribution to the Galactic Bulge Microlensing Optical Depth. ApJ 592, 172–175 (2003). [25] Niikura, H. et al. Microlensing constraints on primordial black holes with Subaru/HSC Andromeda observations. Nature Astronomy 3, 524–534 (2019). [26] Sahu, K. C. Stars within the Large Magellanic Cloud as potential lenses for observed microlensing events. Nature 370, 275–276 (1994). [27] Erkal, D. et al. The total mass of the Large Magellanic Cloud from its perturbation on the Orphan stream. MNRAS 487, 2685–2700 (2019). [28] Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. A&A 678, A208 (2023). [29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. A distance to the Large Magellanic Cloud that is precise to one per cent. Nature 567, 200–203 (2019). [42] Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. An H I Aperture Synthesis Mosaic of the Large Magellanic Cloud. ApJ 503, 674–688 (1998). [44] Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. The dark matter profile of the Milky Way inferred from its circular velocity curve. MNRAS 528, 693–710 (2024). [45] Gaia Collaboration et al. Gaia Data Release 2. 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[39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. A distance to the Large Magellanic Cloud that is precise to one per cent. Nature 567, 200–203 (2019). [42] Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. An H I Aperture Synthesis Mosaic of the Large Magellanic Cloud. ApJ 503, 674–688 (1998). [44] Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. The dark matter profile of the Milky Way inferred from its circular velocity curve. MNRAS 528, 693–710 (2024). [45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. 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[34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. 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Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. 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The Local Group Stellar Populations Archive from the Hubble Space Telescope WFPC2. ApJS 166, 534–548 (2006). [22] Mróz, P. et al. No large population of unbound or wide-orbit Jupiter-mass planets. Nature 548, 183–186 (2017). [23] Cautun, M. et al. The milky way total mass profile as inferred from Gaia DR2. MNRAS 494, 4291–4313 (2020). [24] Han, C. & Gould, A. Stellar Contribution to the Galactic Bulge Microlensing Optical Depth. ApJ 592, 172–175 (2003). [25] Niikura, H. et al. Microlensing constraints on primordial black holes with Subaru/HSC Andromeda observations. Nature Astronomy 3, 524–534 (2019). [26] Sahu, K. C. Stars within the Large Magellanic Cloud as potential lenses for observed microlensing events. Nature 370, 275–276 (1994). [27] Erkal, D. et al. The total mass of the Large Magellanic Cloud from its perturbation on the Orphan stream. MNRAS 487, 2685–2700 (2019). [28] Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. A&A 678, A208 (2023). [29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. A distance to the Large Magellanic Cloud that is precise to one per cent. Nature 567, 200–203 (2019). [42] Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. An H I Aperture Synthesis Mosaic of the Large Magellanic Cloud. ApJ 503, 674–688 (1998). [44] Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. The dark matter profile of the Milky Way inferred from its circular velocity curve. MNRAS 528, 693–710 (2024). [45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021). Clesse, S. & García-Bellido, J. The clustering of massive Primordial Black Holes as Dark Matter: Measuring their mass distribution with advanced LIGO. Phys. Dark Universe 15, 142–147 (2017). [10] Carr, B., Clesse, S., García-Bellido, J. & Kühnel, F. Cosmic conundra explained by thermal history and primordial black holes. Phys. Dark Universe 31, 100755 (2021). [11] Jedamzik, K. Consistency of Primordial Black Hole Dark Matter with LIGO/Virgo Merger Rates. Phys. Rev. Lett. 126, 051302 (2021). [12] Escrivà, A., Bagui, E. & Clesse, S. Simulations of PBH formation at the QCD epoch and comparison with the GWTC-3 catalog. J. Cosmology Astropart. Phys 2023, 004 (2023). [13] Udalski, A., Szymański, M. K. & Szymański, G. OGLE-IV: Fourth Phase of the Optical Gravitational Lensing Experiment. Acta Astron. 65, 1–38 (2015). [14] Paczyński, B. Gravitational microlensing by the galactic halo. ApJ 304, 1–5 (1986). [15] Alcock, C. et al. The MACHO Project: Microlensing Results from 5.7 Years of Large Magellanic Cloud Observations. ApJ 542, 281–307 (2000). [16] Tisserand, P. et al. Limits on the Macho content of the Galactic Halo from the EROS-2 Survey of the Magellanic Clouds. A&A 469, 387–404 (2007). [17] Wyrzykowski, L. et al. The OGLE view of microlensing towards the Magellanic Clouds - IV. OGLE-III SMC data and final conclusions on MACHOs. MNRAS 416, 2949–2961 (2011). [18] Blaineau, T. et al. New limits from microlensing on Galactic black holes in the mass range 10 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT < M < 1000 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT. A&A 664, A106 (2022). [19] Udalski, A. The Optical Gravitational Lensing Experiment. Real Time Data Analysis Systems in the OGLE-III Survey. Acta Astron. 53, 291–305 (2003). [20] Mróz, P. et al. Microlensing optical depth and event rate toward the Large Magellanic Cloud based on 20 years of OGLE observations. submitted (2024). [21] Holtzman, J. A., Afonso, C. & Dolphin, A. The Local Group Stellar Populations Archive from the Hubble Space Telescope WFPC2. ApJS 166, 534–548 (2006). [22] Mróz, P. et al. No large population of unbound or wide-orbit Jupiter-mass planets. Nature 548, 183–186 (2017). [23] Cautun, M. et al. The milky way total mass profile as inferred from Gaia DR2. MNRAS 494, 4291–4313 (2020). [24] Han, C. & Gould, A. Stellar Contribution to the Galactic Bulge Microlensing Optical Depth. ApJ 592, 172–175 (2003). [25] Niikura, H. et al. Microlensing constraints on primordial black holes with Subaru/HSC Andromeda observations. Nature Astronomy 3, 524–534 (2019). [26] Sahu, K. C. Stars within the Large Magellanic Cloud as potential lenses for observed microlensing events. Nature 370, 275–276 (1994). [27] Erkal, D. et al. The total mass of the Large Magellanic Cloud from its perturbation on the Orphan stream. MNRAS 487, 2685–2700 (2019). [28] Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. A&A 678, A208 (2023). [29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. A distance to the Large Magellanic Cloud that is precise to one per cent. Nature 567, 200–203 (2019). [42] Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. An H I Aperture Synthesis Mosaic of the Large Magellanic Cloud. ApJ 503, 674–688 (1998). [44] Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. The dark matter profile of the Milky Way inferred from its circular velocity curve. MNRAS 528, 693–710 (2024). [45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021). Carr, B., Clesse, S., García-Bellido, J. & Kühnel, F. Cosmic conundra explained by thermal history and primordial black holes. Phys. Dark Universe 31, 100755 (2021). [11] Jedamzik, K. Consistency of Primordial Black Hole Dark Matter with LIGO/Virgo Merger Rates. Phys. Rev. Lett. 126, 051302 (2021). [12] Escrivà, A., Bagui, E. & Clesse, S. Simulations of PBH formation at the QCD epoch and comparison with the GWTC-3 catalog. J. Cosmology Astropart. Phys 2023, 004 (2023). [13] Udalski, A., Szymański, M. K. & Szymański, G. OGLE-IV: Fourth Phase of the Optical Gravitational Lensing Experiment. Acta Astron. 65, 1–38 (2015). [14] Paczyński, B. Gravitational microlensing by the galactic halo. ApJ 304, 1–5 (1986). [15] Alcock, C. et al. The MACHO Project: Microlensing Results from 5.7 Years of Large Magellanic Cloud Observations. ApJ 542, 281–307 (2000). [16] Tisserand, P. et al. Limits on the Macho content of the Galactic Halo from the EROS-2 Survey of the Magellanic Clouds. A&A 469, 387–404 (2007). [17] Wyrzykowski, L. et al. The OGLE view of microlensing towards the Magellanic Clouds - IV. OGLE-III SMC data and final conclusions on MACHOs. MNRAS 416, 2949–2961 (2011). [18] Blaineau, T. et al. New limits from microlensing on Galactic black holes in the mass range 10 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT < M < 1000 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT. A&A 664, A106 (2022). [19] Udalski, A. The Optical Gravitational Lensing Experiment. Real Time Data Analysis Systems in the OGLE-III Survey. Acta Astron. 53, 291–305 (2003). [20] Mróz, P. et al. Microlensing optical depth and event rate toward the Large Magellanic Cloud based on 20 years of OGLE observations. submitted (2024). [21] Holtzman, J. A., Afonso, C. & Dolphin, A. The Local Group Stellar Populations Archive from the Hubble Space Telescope WFPC2. ApJS 166, 534–548 (2006). [22] Mróz, P. et al. No large population of unbound or wide-orbit Jupiter-mass planets. Nature 548, 183–186 (2017). [23] Cautun, M. et al. The milky way total mass profile as inferred from Gaia DR2. MNRAS 494, 4291–4313 (2020). [24] Han, C. & Gould, A. Stellar Contribution to the Galactic Bulge Microlensing Optical Depth. ApJ 592, 172–175 (2003). [25] Niikura, H. et al. Microlensing constraints on primordial black holes with Subaru/HSC Andromeda observations. Nature Astronomy 3, 524–534 (2019). [26] Sahu, K. C. Stars within the Large Magellanic Cloud as potential lenses for observed microlensing events. Nature 370, 275–276 (1994). [27] Erkal, D. et al. The total mass of the Large Magellanic Cloud from its perturbation on the Orphan stream. MNRAS 487, 2685–2700 (2019). [28] Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. A&A 678, A208 (2023). [29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. A distance to the Large Magellanic Cloud that is precise to one per cent. Nature 567, 200–203 (2019). [42] Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. An H I Aperture Synthesis Mosaic of the Large Magellanic Cloud. ApJ 503, 674–688 (1998). [44] Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. The dark matter profile of the Milky Way inferred from its circular velocity curve. MNRAS 528, 693–710 (2024). [45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021). Jedamzik, K. Consistency of Primordial Black Hole Dark Matter with LIGO/Virgo Merger Rates. Phys. Rev. Lett. 126, 051302 (2021). [12] Escrivà, A., Bagui, E. & Clesse, S. Simulations of PBH formation at the QCD epoch and comparison with the GWTC-3 catalog. J. Cosmology Astropart. Phys 2023, 004 (2023). [13] Udalski, A., Szymański, M. K. & Szymański, G. OGLE-IV: Fourth Phase of the Optical Gravitational Lensing Experiment. Acta Astron. 65, 1–38 (2015). [14] Paczyński, B. Gravitational microlensing by the galactic halo. ApJ 304, 1–5 (1986). [15] Alcock, C. et al. The MACHO Project: Microlensing Results from 5.7 Years of Large Magellanic Cloud Observations. ApJ 542, 281–307 (2000). [16] Tisserand, P. et al. Limits on the Macho content of the Galactic Halo from the EROS-2 Survey of the Magellanic Clouds. A&A 469, 387–404 (2007). [17] Wyrzykowski, L. et al. The OGLE view of microlensing towards the Magellanic Clouds - IV. OGLE-III SMC data and final conclusions on MACHOs. MNRAS 416, 2949–2961 (2011). [18] Blaineau, T. et al. New limits from microlensing on Galactic black holes in the mass range 10 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT < M < 1000 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT. A&A 664, A106 (2022). [19] Udalski, A. The Optical Gravitational Lensing Experiment. Real Time Data Analysis Systems in the OGLE-III Survey. Acta Astron. 53, 291–305 (2003). [20] Mróz, P. et al. Microlensing optical depth and event rate toward the Large Magellanic Cloud based on 20 years of OGLE observations. submitted (2024). [21] Holtzman, J. A., Afonso, C. & Dolphin, A. The Local Group Stellar Populations Archive from the Hubble Space Telescope WFPC2. ApJS 166, 534–548 (2006). [22] Mróz, P. et al. No large population of unbound or wide-orbit Jupiter-mass planets. Nature 548, 183–186 (2017). [23] Cautun, M. et al. The milky way total mass profile as inferred from Gaia DR2. MNRAS 494, 4291–4313 (2020). [24] Han, C. & Gould, A. Stellar Contribution to the Galactic Bulge Microlensing Optical Depth. ApJ 592, 172–175 (2003). [25] Niikura, H. et al. Microlensing constraints on primordial black holes with Subaru/HSC Andromeda observations. Nature Astronomy 3, 524–534 (2019). [26] Sahu, K. C. Stars within the Large Magellanic Cloud as potential lenses for observed microlensing events. Nature 370, 275–276 (1994). [27] Erkal, D. et al. The total mass of the Large Magellanic Cloud from its perturbation on the Orphan stream. MNRAS 487, 2685–2700 (2019). [28] Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. A&A 678, A208 (2023). [29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. A distance to the Large Magellanic Cloud that is precise to one per cent. Nature 567, 200–203 (2019). [42] Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. An H I Aperture Synthesis Mosaic of the Large Magellanic Cloud. ApJ 503, 674–688 (1998). [44] Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. The dark matter profile of the Milky Way inferred from its circular velocity curve. MNRAS 528, 693–710 (2024). [45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021). Escrivà, A., Bagui, E. & Clesse, S. Simulations of PBH formation at the QCD epoch and comparison with the GWTC-3 catalog. J. Cosmology Astropart. Phys 2023, 004 (2023). [13] Udalski, A., Szymański, M. K. & Szymański, G. OGLE-IV: Fourth Phase of the Optical Gravitational Lensing Experiment. Acta Astron. 65, 1–38 (2015). [14] Paczyński, B. Gravitational microlensing by the galactic halo. ApJ 304, 1–5 (1986). [15] Alcock, C. et al. The MACHO Project: Microlensing Results from 5.7 Years of Large Magellanic Cloud Observations. ApJ 542, 281–307 (2000). [16] Tisserand, P. et al. Limits on the Macho content of the Galactic Halo from the EROS-2 Survey of the Magellanic Clouds. A&A 469, 387–404 (2007). [17] Wyrzykowski, L. et al. The OGLE view of microlensing towards the Magellanic Clouds - IV. OGLE-III SMC data and final conclusions on MACHOs. MNRAS 416, 2949–2961 (2011). [18] Blaineau, T. et al. New limits from microlensing on Galactic black holes in the mass range 10 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT < M < 1000 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT. A&A 664, A106 (2022). [19] Udalski, A. The Optical Gravitational Lensing Experiment. Real Time Data Analysis Systems in the OGLE-III Survey. Acta Astron. 53, 291–305 (2003). [20] Mróz, P. et al. Microlensing optical depth and event rate toward the Large Magellanic Cloud based on 20 years of OGLE observations. submitted (2024). [21] Holtzman, J. A., Afonso, C. & Dolphin, A. The Local Group Stellar Populations Archive from the Hubble Space Telescope WFPC2. ApJS 166, 534–548 (2006). [22] Mróz, P. et al. No large population of unbound or wide-orbit Jupiter-mass planets. Nature 548, 183–186 (2017). [23] Cautun, M. et al. The milky way total mass profile as inferred from Gaia DR2. MNRAS 494, 4291–4313 (2020). [24] Han, C. & Gould, A. Stellar Contribution to the Galactic Bulge Microlensing Optical Depth. ApJ 592, 172–175 (2003). [25] Niikura, H. et al. Microlensing constraints on primordial black holes with Subaru/HSC Andromeda observations. Nature Astronomy 3, 524–534 (2019). [26] Sahu, K. C. Stars within the Large Magellanic Cloud as potential lenses for observed microlensing events. Nature 370, 275–276 (1994). [27] Erkal, D. et al. The total mass of the Large Magellanic Cloud from its perturbation on the Orphan stream. MNRAS 487, 2685–2700 (2019). [28] Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. A&A 678, A208 (2023). [29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. A distance to the Large Magellanic Cloud that is precise to one per cent. Nature 567, 200–203 (2019). [42] Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. An H I Aperture Synthesis Mosaic of the Large Magellanic Cloud. ApJ 503, 674–688 (1998). [44] Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. The dark matter profile of the Milky Way inferred from its circular velocity curve. MNRAS 528, 693–710 (2024). [45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021). Udalski, A., Szymański, M. K. & Szymański, G. OGLE-IV: Fourth Phase of the Optical Gravitational Lensing Experiment. Acta Astron. 65, 1–38 (2015). [14] Paczyński, B. Gravitational microlensing by the galactic halo. ApJ 304, 1–5 (1986). [15] Alcock, C. et al. The MACHO Project: Microlensing Results from 5.7 Years of Large Magellanic Cloud Observations. ApJ 542, 281–307 (2000). [16] Tisserand, P. et al. Limits on the Macho content of the Galactic Halo from the EROS-2 Survey of the Magellanic Clouds. A&A 469, 387–404 (2007). [17] Wyrzykowski, L. et al. The OGLE view of microlensing towards the Magellanic Clouds - IV. OGLE-III SMC data and final conclusions on MACHOs. MNRAS 416, 2949–2961 (2011). [18] Blaineau, T. et al. New limits from microlensing on Galactic black holes in the mass range 10 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT < M < 1000 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT. A&A 664, A106 (2022). [19] Udalski, A. The Optical Gravitational Lensing Experiment. Real Time Data Analysis Systems in the OGLE-III Survey. Acta Astron. 53, 291–305 (2003). [20] Mróz, P. et al. Microlensing optical depth and event rate toward the Large Magellanic Cloud based on 20 years of OGLE observations. submitted (2024). [21] Holtzman, J. A., Afonso, C. & Dolphin, A. The Local Group Stellar Populations Archive from the Hubble Space Telescope WFPC2. ApJS 166, 534–548 (2006). [22] Mróz, P. et al. No large population of unbound or wide-orbit Jupiter-mass planets. Nature 548, 183–186 (2017). [23] Cautun, M. et al. The milky way total mass profile as inferred from Gaia DR2. MNRAS 494, 4291–4313 (2020). [24] Han, C. & Gould, A. Stellar Contribution to the Galactic Bulge Microlensing Optical Depth. ApJ 592, 172–175 (2003). [25] Niikura, H. et al. Microlensing constraints on primordial black holes with Subaru/HSC Andromeda observations. Nature Astronomy 3, 524–534 (2019). [26] Sahu, K. C. Stars within the Large Magellanic Cloud as potential lenses for observed microlensing events. Nature 370, 275–276 (1994). [27] Erkal, D. et al. The total mass of the Large Magellanic Cloud from its perturbation on the Orphan stream. MNRAS 487, 2685–2700 (2019). [28] Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. A&A 678, A208 (2023). [29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. 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A&A 664, A106 (2022). [19] Udalski, A. The Optical Gravitational Lensing Experiment. Real Time Data Analysis Systems in the OGLE-III Survey. Acta Astron. 53, 291–305 (2003). [20] Mróz, P. et al. Microlensing optical depth and event rate toward the Large Magellanic Cloud based on 20 years of OGLE observations. submitted (2024). [21] Holtzman, J. A., Afonso, C. & Dolphin, A. The Local Group Stellar Populations Archive from the Hubble Space Telescope WFPC2. ApJS 166, 534–548 (2006). [22] Mróz, P. et al. No large population of unbound or wide-orbit Jupiter-mass planets. Nature 548, 183–186 (2017). [23] Cautun, M. et al. The milky way total mass profile as inferred from Gaia DR2. MNRAS 494, 4291–4313 (2020). [24] Han, C. & Gould, A. Stellar Contribution to the Galactic Bulge Microlensing Optical Depth. ApJ 592, 172–175 (2003). [25] Niikura, H. et al. Microlensing constraints on primordial black holes with Subaru/HSC Andromeda observations. Nature Astronomy 3, 524–534 (2019). [26] Sahu, K. C. Stars within the Large Magellanic Cloud as potential lenses for observed microlensing events. Nature 370, 275–276 (1994). [27] Erkal, D. et al. The total mass of the Large Magellanic Cloud from its perturbation on the Orphan stream. MNRAS 487, 2685–2700 (2019). [28] Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. A&A 678, A208 (2023). [29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. 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The Local Group Stellar Populations Archive from the Hubble Space Telescope WFPC2. ApJS 166, 534–548 (2006). [22] Mróz, P. et al. No large population of unbound or wide-orbit Jupiter-mass planets. Nature 548, 183–186 (2017). [23] Cautun, M. et al. The milky way total mass profile as inferred from Gaia DR2. MNRAS 494, 4291–4313 (2020). [24] Han, C. & Gould, A. Stellar Contribution to the Galactic Bulge Microlensing Optical Depth. ApJ 592, 172–175 (2003). [25] Niikura, H. et al. Microlensing constraints on primordial black holes with Subaru/HSC Andromeda observations. Nature Astronomy 3, 524–534 (2019). [26] Sahu, K. C. Stars within the Large Magellanic Cloud as potential lenses for observed microlensing events. Nature 370, 275–276 (1994). [27] Erkal, D. et al. The total mass of the Large Magellanic Cloud from its perturbation on the Orphan stream. MNRAS 487, 2685–2700 (2019). [28] Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. A&A 678, A208 (2023). [29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. A distance to the Large Magellanic Cloud that is precise to one per cent. Nature 567, 200–203 (2019). [42] Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. An H I Aperture Synthesis Mosaic of the Large Magellanic Cloud. ApJ 503, 674–688 (1998). [44] Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. The dark matter profile of the Milky Way inferred from its circular velocity curve. MNRAS 528, 693–710 (2024). [45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021). Tisserand, P. et al. Limits on the Macho content of the Galactic Halo from the EROS-2 Survey of the Magellanic Clouds. A&A 469, 387–404 (2007). [17] Wyrzykowski, L. et al. The OGLE view of microlensing towards the Magellanic Clouds - IV. OGLE-III SMC data and final conclusions on MACHOs. MNRAS 416, 2949–2961 (2011). [18] Blaineau, T. et al. New limits from microlensing on Galactic black holes in the mass range 10 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT < M < 1000 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT. A&A 664, A106 (2022). [19] Udalski, A. The Optical Gravitational Lensing Experiment. Real Time Data Analysis Systems in the OGLE-III Survey. Acta Astron. 53, 291–305 (2003). [20] Mróz, P. et al. Microlensing optical depth and event rate toward the Large Magellanic Cloud based on 20 years of OGLE observations. submitted (2024). [21] Holtzman, J. A., Afonso, C. & Dolphin, A. The Local Group Stellar Populations Archive from the Hubble Space Telescope WFPC2. ApJS 166, 534–548 (2006). [22] Mróz, P. et al. No large population of unbound or wide-orbit Jupiter-mass planets. Nature 548, 183–186 (2017). [23] Cautun, M. et al. The milky way total mass profile as inferred from Gaia DR2. MNRAS 494, 4291–4313 (2020). [24] Han, C. & Gould, A. Stellar Contribution to the Galactic Bulge Microlensing Optical Depth. ApJ 592, 172–175 (2003). [25] Niikura, H. et al. Microlensing constraints on primordial black holes with Subaru/HSC Andromeda observations. Nature Astronomy 3, 524–534 (2019). [26] Sahu, K. C. Stars within the Large Magellanic Cloud as potential lenses for observed microlensing events. Nature 370, 275–276 (1994). [27] Erkal, D. et al. The total mass of the Large Magellanic Cloud from its perturbation on the Orphan stream. MNRAS 487, 2685–2700 (2019). [28] Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. A&A 678, A208 (2023). [29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. A distance to the Large Magellanic Cloud that is precise to one per cent. Nature 567, 200–203 (2019). [42] Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. An H I Aperture Synthesis Mosaic of the Large Magellanic Cloud. ApJ 503, 674–688 (1998). [44] Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. The dark matter profile of the Milky Way inferred from its circular velocity curve. MNRAS 528, 693–710 (2024). [45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021). Wyrzykowski, L. et al. The OGLE view of microlensing towards the Magellanic Clouds - IV. OGLE-III SMC data and final conclusions on MACHOs. MNRAS 416, 2949–2961 (2011). [18] Blaineau, T. et al. New limits from microlensing on Galactic black holes in the mass range 10 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT < M < 1000 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT. A&A 664, A106 (2022). [19] Udalski, A. The Optical Gravitational Lensing Experiment. Real Time Data Analysis Systems in the OGLE-III Survey. Acta Astron. 53, 291–305 (2003). [20] Mróz, P. et al. Microlensing optical depth and event rate toward the Large Magellanic Cloud based on 20 years of OGLE observations. submitted (2024). [21] Holtzman, J. A., Afonso, C. & Dolphin, A. The Local Group Stellar Populations Archive from the Hubble Space Telescope WFPC2. ApJS 166, 534–548 (2006). [22] Mróz, P. et al. No large population of unbound or wide-orbit Jupiter-mass planets. Nature 548, 183–186 (2017). [23] Cautun, M. et al. The milky way total mass profile as inferred from Gaia DR2. MNRAS 494, 4291–4313 (2020). [24] Han, C. & Gould, A. Stellar Contribution to the Galactic Bulge Microlensing Optical Depth. ApJ 592, 172–175 (2003). [25] Niikura, H. et al. Microlensing constraints on primordial black holes with Subaru/HSC Andromeda observations. Nature Astronomy 3, 524–534 (2019). [26] Sahu, K. C. Stars within the Large Magellanic Cloud as potential lenses for observed microlensing events. Nature 370, 275–276 (1994). [27] Erkal, D. et al. The total mass of the Large Magellanic Cloud from its perturbation on the Orphan stream. MNRAS 487, 2685–2700 (2019). [28] Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. A&A 678, A208 (2023). [29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. A distance to the Large Magellanic Cloud that is precise to one per cent. Nature 567, 200–203 (2019). [42] Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. An H I Aperture Synthesis Mosaic of the Large Magellanic Cloud. ApJ 503, 674–688 (1998). [44] Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. The dark matter profile of the Milky Way inferred from its circular velocity curve. MNRAS 528, 693–710 (2024). [45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021). Blaineau, T. et al. New limits from microlensing on Galactic black holes in the mass range 10 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT < M < 1000 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT. A&A 664, A106 (2022). [19] Udalski, A. The Optical Gravitational Lensing Experiment. Real Time Data Analysis Systems in the OGLE-III Survey. Acta Astron. 53, 291–305 (2003). [20] Mróz, P. et al. Microlensing optical depth and event rate toward the Large Magellanic Cloud based on 20 years of OGLE observations. submitted (2024). [21] Holtzman, J. A., Afonso, C. & Dolphin, A. The Local Group Stellar Populations Archive from the Hubble Space Telescope WFPC2. ApJS 166, 534–548 (2006). [22] Mróz, P. et al. No large population of unbound or wide-orbit Jupiter-mass planets. Nature 548, 183–186 (2017). [23] Cautun, M. et al. The milky way total mass profile as inferred from Gaia DR2. MNRAS 494, 4291–4313 (2020). [24] Han, C. & Gould, A. Stellar Contribution to the Galactic Bulge Microlensing Optical Depth. ApJ 592, 172–175 (2003). [25] Niikura, H. et al. Microlensing constraints on primordial black holes with Subaru/HSC Andromeda observations. Nature Astronomy 3, 524–534 (2019). [26] Sahu, K. C. Stars within the Large Magellanic Cloud as potential lenses for observed microlensing events. Nature 370, 275–276 (1994). [27] Erkal, D. et al. 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[29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. A distance to the Large Magellanic Cloud that is precise to one per cent. Nature 567, 200–203 (2019). [42] Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. 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[25] Niikura, H. et al. Microlensing constraints on primordial black holes with Subaru/HSC Andromeda observations. Nature Astronomy 3, 524–534 (2019). [26] Sahu, K. C. Stars within the Large Magellanic Cloud as potential lenses for observed microlensing events. Nature 370, 275–276 (1994). [27] Erkal, D. et al. The total mass of the Large Magellanic Cloud from its perturbation on the Orphan stream. MNRAS 487, 2685–2700 (2019). [28] Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. A&A 678, A208 (2023). [29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. A distance to the Large Magellanic Cloud that is precise to one per cent. Nature 567, 200–203 (2019). [42] Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. An H I Aperture Synthesis Mosaic of the Large Magellanic Cloud. ApJ 503, 674–688 (1998). [44] Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. The dark matter profile of the Milky Way inferred from its circular velocity curve. MNRAS 528, 693–710 (2024). [45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. 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Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. 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The total mass of the Large Magellanic Cloud from its perturbation on the Orphan stream. MNRAS 487, 2685–2700 (2019). [28] Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. A&A 678, A208 (2023). [29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. A distance to the Large Magellanic Cloud that is precise to one per cent. Nature 567, 200–203 (2019). [42] Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. An H I Aperture Synthesis Mosaic of the Large Magellanic Cloud. ApJ 503, 674–688 (1998). [44] Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. The dark matter profile of the Milky Way inferred from its circular velocity curve. MNRAS 528, 693–710 (2024). [45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021). Han, C. & Gould, A. Stellar Contribution to the Galactic Bulge Microlensing Optical Depth. ApJ 592, 172–175 (2003). [25] Niikura, H. et al. Microlensing constraints on primordial black holes with Subaru/HSC Andromeda observations. Nature Astronomy 3, 524–534 (2019). [26] Sahu, K. C. Stars within the Large Magellanic Cloud as potential lenses for observed microlensing events. Nature 370, 275–276 (1994). [27] Erkal, D. et al. The total mass of the Large Magellanic Cloud from its perturbation on the Orphan stream. MNRAS 487, 2685–2700 (2019). [28] Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. A&A 678, A208 (2023). [29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. A distance to the Large Magellanic Cloud that is precise to one per cent. Nature 567, 200–203 (2019). [42] Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. An H I Aperture Synthesis Mosaic of the Large Magellanic Cloud. ApJ 503, 674–688 (1998). [44] Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. The dark matter profile of the Milky Way inferred from its circular velocity curve. MNRAS 528, 693–710 (2024). [45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021). Niikura, H. et al. Microlensing constraints on primordial black holes with Subaru/HSC Andromeda observations. 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[45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021). Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. 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[45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021). Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. 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[12] Escrivà, A., Bagui, E. & Clesse, S. Simulations of PBH formation at the QCD epoch and comparison with the GWTC-3 catalog. J. Cosmology Astropart. Phys 2023, 004 (2023). [13] Udalski, A., Szymański, M. K. & Szymański, G. OGLE-IV: Fourth Phase of the Optical Gravitational Lensing Experiment. Acta Astron. 65, 1–38 (2015). [14] Paczyński, B. Gravitational microlensing by the galactic halo. ApJ 304, 1–5 (1986). [15] Alcock, C. et al. The MACHO Project: Microlensing Results from 5.7 Years of Large Magellanic Cloud Observations. ApJ 542, 281–307 (2000). [16] Tisserand, P. et al. Limits on the Macho content of the Galactic Halo from the EROS-2 Survey of the Magellanic Clouds. A&A 469, 387–404 (2007). [17] Wyrzykowski, L. et al. The OGLE view of microlensing towards the Magellanic Clouds - IV. OGLE-III SMC data and final conclusions on MACHOs. MNRAS 416, 2949–2961 (2011). [18] Blaineau, T. et al. New limits from microlensing on Galactic black holes in the mass range 10 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT < M < 1000 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT. A&A 664, A106 (2022). [19] Udalski, A. The Optical Gravitational Lensing Experiment. Real Time Data Analysis Systems in the OGLE-III Survey. Acta Astron. 53, 291–305 (2003). [20] Mróz, P. et al. Microlensing optical depth and event rate toward the Large Magellanic Cloud based on 20 years of OGLE observations. submitted (2024). [21] Holtzman, J. A., Afonso, C. & Dolphin, A. The Local Group Stellar Populations Archive from the Hubble Space Telescope WFPC2. ApJS 166, 534–548 (2006). [22] Mróz, P. et al. No large population of unbound or wide-orbit Jupiter-mass planets. Nature 548, 183–186 (2017). [23] Cautun, M. et al. The milky way total mass profile as inferred from Gaia DR2. MNRAS 494, 4291–4313 (2020). [24] Han, C. & Gould, A. Stellar Contribution to the Galactic Bulge Microlensing Optical Depth. ApJ 592, 172–175 (2003). [25] Niikura, H. et al. Microlensing constraints on primordial black holes with Subaru/HSC Andromeda observations. Nature Astronomy 3, 524–534 (2019). [26] Sahu, K. C. Stars within the Large Magellanic Cloud as potential lenses for observed microlensing events. Nature 370, 275–276 (1994). [27] Erkal, D. et al. The total mass of the Large Magellanic Cloud from its perturbation on the Orphan stream. MNRAS 487, 2685–2700 (2019). [28] Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. A&A 678, A208 (2023). [29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. A distance to the Large Magellanic Cloud that is precise to one per cent. Nature 567, 200–203 (2019). [42] Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. An H I Aperture Synthesis Mosaic of the Large Magellanic Cloud. ApJ 503, 674–688 (1998). [44] Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. The dark matter profile of the Milky Way inferred from its circular velocity curve. MNRAS 528, 693–710 (2024). [45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021). Sasaki, M., Suyama, T., Tanaka, T. & Yokoyama, S. Primordial Black Hole Scenario for the Gravitational-Wave Event GW150914. Phys. Rev. Lett. 117, 061101 (2016). [9] Clesse, S. & García-Bellido, J. The clustering of massive Primordial Black Holes as Dark Matter: Measuring their mass distribution with advanced LIGO. Phys. Dark Universe 15, 142–147 (2017). [10] Carr, B., Clesse, S., García-Bellido, J. & Kühnel, F. Cosmic conundra explained by thermal history and primordial black holes. Phys. Dark Universe 31, 100755 (2021). [11] Jedamzik, K. Consistency of Primordial Black Hole Dark Matter with LIGO/Virgo Merger Rates. Phys. Rev. Lett. 126, 051302 (2021). [12] Escrivà, A., Bagui, E. & Clesse, S. Simulations of PBH formation at the QCD epoch and comparison with the GWTC-3 catalog. J. Cosmology Astropart. Phys 2023, 004 (2023). [13] Udalski, A., Szymański, M. K. & Szymański, G. OGLE-IV: Fourth Phase of the Optical Gravitational Lensing Experiment. Acta Astron. 65, 1–38 (2015). [14] Paczyński, B. Gravitational microlensing by the galactic halo. ApJ 304, 1–5 (1986). [15] Alcock, C. et al. The MACHO Project: Microlensing Results from 5.7 Years of Large Magellanic Cloud Observations. ApJ 542, 281–307 (2000). [16] Tisserand, P. et al. Limits on the Macho content of the Galactic Halo from the EROS-2 Survey of the Magellanic Clouds. A&A 469, 387–404 (2007). [17] Wyrzykowski, L. et al. The OGLE view of microlensing towards the Magellanic Clouds - IV. OGLE-III SMC data and final conclusions on MACHOs. MNRAS 416, 2949–2961 (2011). [18] Blaineau, T. et al. New limits from microlensing on Galactic black holes in the mass range 10 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT < M < 1000 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT. A&A 664, A106 (2022). [19] Udalski, A. The Optical Gravitational Lensing Experiment. Real Time Data Analysis Systems in the OGLE-III Survey. Acta Astron. 53, 291–305 (2003). [20] Mróz, P. et al. Microlensing optical depth and event rate toward the Large Magellanic Cloud based on 20 years of OGLE observations. submitted (2024). [21] Holtzman, J. A., Afonso, C. & Dolphin, A. The Local Group Stellar Populations Archive from the Hubble Space Telescope WFPC2. ApJS 166, 534–548 (2006). [22] Mróz, P. et al. No large population of unbound or wide-orbit Jupiter-mass planets. Nature 548, 183–186 (2017). [23] Cautun, M. et al. The milky way total mass profile as inferred from Gaia DR2. MNRAS 494, 4291–4313 (2020). [24] Han, C. & Gould, A. Stellar Contribution to the Galactic Bulge Microlensing Optical Depth. ApJ 592, 172–175 (2003). [25] Niikura, H. et al. Microlensing constraints on primordial black holes with Subaru/HSC Andromeda observations. Nature Astronomy 3, 524–534 (2019). [26] Sahu, K. C. Stars within the Large Magellanic Cloud as potential lenses for observed microlensing events. Nature 370, 275–276 (1994). [27] Erkal, D. et al. The total mass of the Large Magellanic Cloud from its perturbation on the Orphan stream. MNRAS 487, 2685–2700 (2019). [28] Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. A&A 678, A208 (2023). [29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. A distance to the Large Magellanic Cloud that is precise to one per cent. Nature 567, 200–203 (2019). [42] Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. An H I Aperture Synthesis Mosaic of the Large Magellanic Cloud. ApJ 503, 674–688 (1998). [44] Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. The dark matter profile of the Milky Way inferred from its circular velocity curve. MNRAS 528, 693–710 (2024). [45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021). Clesse, S. & García-Bellido, J. The clustering of massive Primordial Black Holes as Dark Matter: Measuring their mass distribution with advanced LIGO. Phys. Dark Universe 15, 142–147 (2017). [10] Carr, B., Clesse, S., García-Bellido, J. & Kühnel, F. Cosmic conundra explained by thermal history and primordial black holes. Phys. Dark Universe 31, 100755 (2021). [11] Jedamzik, K. Consistency of Primordial Black Hole Dark Matter with LIGO/Virgo Merger Rates. Phys. Rev. Lett. 126, 051302 (2021). [12] Escrivà, A., Bagui, E. & Clesse, S. Simulations of PBH formation at the QCD epoch and comparison with the GWTC-3 catalog. J. Cosmology Astropart. Phys 2023, 004 (2023). [13] Udalski, A., Szymański, M. K. & Szymański, G. OGLE-IV: Fourth Phase of the Optical Gravitational Lensing Experiment. Acta Astron. 65, 1–38 (2015). [14] Paczyński, B. Gravitational microlensing by the galactic halo. ApJ 304, 1–5 (1986). [15] Alcock, C. et al. The MACHO Project: Microlensing Results from 5.7 Years of Large Magellanic Cloud Observations. ApJ 542, 281–307 (2000). [16] Tisserand, P. et al. Limits on the Macho content of the Galactic Halo from the EROS-2 Survey of the Magellanic Clouds. A&A 469, 387–404 (2007). [17] Wyrzykowski, L. et al. The OGLE view of microlensing towards the Magellanic Clouds - IV. OGLE-III SMC data and final conclusions on MACHOs. MNRAS 416, 2949–2961 (2011). [18] Blaineau, T. et al. New limits from microlensing on Galactic black holes in the mass range 10 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT < M < 1000 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT. A&A 664, A106 (2022). [19] Udalski, A. The Optical Gravitational Lensing Experiment. Real Time Data Analysis Systems in the OGLE-III Survey. Acta Astron. 53, 291–305 (2003). [20] Mróz, P. et al. Microlensing optical depth and event rate toward the Large Magellanic Cloud based on 20 years of OGLE observations. submitted (2024). [21] Holtzman, J. A., Afonso, C. & Dolphin, A. The Local Group Stellar Populations Archive from the Hubble Space Telescope WFPC2. ApJS 166, 534–548 (2006). [22] Mróz, P. et al. No large population of unbound or wide-orbit Jupiter-mass planets. Nature 548, 183–186 (2017). [23] Cautun, M. et al. The milky way total mass profile as inferred from Gaia DR2. MNRAS 494, 4291–4313 (2020). [24] Han, C. & Gould, A. Stellar Contribution to the Galactic Bulge Microlensing Optical Depth. ApJ 592, 172–175 (2003). [25] Niikura, H. et al. Microlensing constraints on primordial black holes with Subaru/HSC Andromeda observations. Nature Astronomy 3, 524–534 (2019). [26] Sahu, K. C. Stars within the Large Magellanic Cloud as potential lenses for observed microlensing events. Nature 370, 275–276 (1994). [27] Erkal, D. et al. The total mass of the Large Magellanic Cloud from its perturbation on the Orphan stream. MNRAS 487, 2685–2700 (2019). [28] Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. A&A 678, A208 (2023). [29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. A distance to the Large Magellanic Cloud that is precise to one per cent. Nature 567, 200–203 (2019). [42] Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. An H I Aperture Synthesis Mosaic of the Large Magellanic Cloud. ApJ 503, 674–688 (1998). [44] Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. The dark matter profile of the Milky Way inferred from its circular velocity curve. MNRAS 528, 693–710 (2024). [45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021). Carr, B., Clesse, S., García-Bellido, J. & Kühnel, F. Cosmic conundra explained by thermal history and primordial black holes. Phys. Dark Universe 31, 100755 (2021). [11] Jedamzik, K. Consistency of Primordial Black Hole Dark Matter with LIGO/Virgo Merger Rates. Phys. Rev. Lett. 126, 051302 (2021). [12] Escrivà, A., Bagui, E. & Clesse, S. Simulations of PBH formation at the QCD epoch and comparison with the GWTC-3 catalog. J. Cosmology Astropart. Phys 2023, 004 (2023). [13] Udalski, A., Szymański, M. K. & Szymański, G. OGLE-IV: Fourth Phase of the Optical Gravitational Lensing Experiment. Acta Astron. 65, 1–38 (2015). [14] Paczyński, B. Gravitational microlensing by the galactic halo. ApJ 304, 1–5 (1986). [15] Alcock, C. et al. The MACHO Project: Microlensing Results from 5.7 Years of Large Magellanic Cloud Observations. ApJ 542, 281–307 (2000). [16] Tisserand, P. et al. Limits on the Macho content of the Galactic Halo from the EROS-2 Survey of the Magellanic Clouds. A&A 469, 387–404 (2007). [17] Wyrzykowski, L. et al. The OGLE view of microlensing towards the Magellanic Clouds - IV. OGLE-III SMC data and final conclusions on MACHOs. MNRAS 416, 2949–2961 (2011). [18] Blaineau, T. et al. New limits from microlensing on Galactic black holes in the mass range 10 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT < M < 1000 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT. A&A 664, A106 (2022). [19] Udalski, A. The Optical Gravitational Lensing Experiment. Real Time Data Analysis Systems in the OGLE-III Survey. Acta Astron. 53, 291–305 (2003). [20] Mróz, P. et al. Microlensing optical depth and event rate toward the Large Magellanic Cloud based on 20 years of OGLE observations. submitted (2024). [21] Holtzman, J. A., Afonso, C. & Dolphin, A. The Local Group Stellar Populations Archive from the Hubble Space Telescope WFPC2. ApJS 166, 534–548 (2006). [22] Mróz, P. et al. No large population of unbound or wide-orbit Jupiter-mass planets. Nature 548, 183–186 (2017). [23] Cautun, M. et al. The milky way total mass profile as inferred from Gaia DR2. MNRAS 494, 4291–4313 (2020). [24] Han, C. & Gould, A. Stellar Contribution to the Galactic Bulge Microlensing Optical Depth. ApJ 592, 172–175 (2003). [25] Niikura, H. et al. Microlensing constraints on primordial black holes with Subaru/HSC Andromeda observations. Nature Astronomy 3, 524–534 (2019). [26] Sahu, K. C. Stars within the Large Magellanic Cloud as potential lenses for observed microlensing events. Nature 370, 275–276 (1994). [27] Erkal, D. et al. The total mass of the Large Magellanic Cloud from its perturbation on the Orphan stream. MNRAS 487, 2685–2700 (2019). [28] Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. A&A 678, A208 (2023). [29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. A distance to the Large Magellanic Cloud that is precise to one per cent. Nature 567, 200–203 (2019). [42] Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. An H I Aperture Synthesis Mosaic of the Large Magellanic Cloud. ApJ 503, 674–688 (1998). [44] Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. The dark matter profile of the Milky Way inferred from its circular velocity curve. MNRAS 528, 693–710 (2024). [45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021). Jedamzik, K. Consistency of Primordial Black Hole Dark Matter with LIGO/Virgo Merger Rates. Phys. Rev. Lett. 126, 051302 (2021). [12] Escrivà, A., Bagui, E. & Clesse, S. Simulations of PBH formation at the QCD epoch and comparison with the GWTC-3 catalog. J. Cosmology Astropart. Phys 2023, 004 (2023). [13] Udalski, A., Szymański, M. K. & Szymański, G. OGLE-IV: Fourth Phase of the Optical Gravitational Lensing Experiment. Acta Astron. 65, 1–38 (2015). [14] Paczyński, B. Gravitational microlensing by the galactic halo. ApJ 304, 1–5 (1986). [15] Alcock, C. et al. The MACHO Project: Microlensing Results from 5.7 Years of Large Magellanic Cloud Observations. ApJ 542, 281–307 (2000). [16] Tisserand, P. et al. Limits on the Macho content of the Galactic Halo from the EROS-2 Survey of the Magellanic Clouds. A&A 469, 387–404 (2007). [17] Wyrzykowski, L. et al. The OGLE view of microlensing towards the Magellanic Clouds - IV. OGLE-III SMC data and final conclusions on MACHOs. MNRAS 416, 2949–2961 (2011). [18] Blaineau, T. et al. New limits from microlensing on Galactic black holes in the mass range 10 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT < M < 1000 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT. A&A 664, A106 (2022). [19] Udalski, A. The Optical Gravitational Lensing Experiment. Real Time Data Analysis Systems in the OGLE-III Survey. Acta Astron. 53, 291–305 (2003). [20] Mróz, P. et al. Microlensing optical depth and event rate toward the Large Magellanic Cloud based on 20 years of OGLE observations. submitted (2024). [21] Holtzman, J. A., Afonso, C. & Dolphin, A. The Local Group Stellar Populations Archive from the Hubble Space Telescope WFPC2. ApJS 166, 534–548 (2006). [22] Mróz, P. et al. No large population of unbound or wide-orbit Jupiter-mass planets. Nature 548, 183–186 (2017). [23] Cautun, M. et al. The milky way total mass profile as inferred from Gaia DR2. MNRAS 494, 4291–4313 (2020). [24] Han, C. & Gould, A. Stellar Contribution to the Galactic Bulge Microlensing Optical Depth. ApJ 592, 172–175 (2003). [25] Niikura, H. et al. Microlensing constraints on primordial black holes with Subaru/HSC Andromeda observations. Nature Astronomy 3, 524–534 (2019). [26] Sahu, K. C. Stars within the Large Magellanic Cloud as potential lenses for observed microlensing events. Nature 370, 275–276 (1994). [27] Erkal, D. et al. The total mass of the Large Magellanic Cloud from its perturbation on the Orphan stream. MNRAS 487, 2685–2700 (2019). [28] Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. A&A 678, A208 (2023). 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Microlensing optical depth and event rate toward the Large Magellanic Cloud based on 20 years of OGLE observations. submitted (2024). [21] Holtzman, J. A., Afonso, C. & Dolphin, A. The Local Group Stellar Populations Archive from the Hubble Space Telescope WFPC2. ApJS 166, 534–548 (2006). [22] Mróz, P. et al. No large population of unbound or wide-orbit Jupiter-mass planets. Nature 548, 183–186 (2017). [23] Cautun, M. et al. The milky way total mass profile as inferred from Gaia DR2. MNRAS 494, 4291–4313 (2020). [24] Han, C. & Gould, A. Stellar Contribution to the Galactic Bulge Microlensing Optical Depth. ApJ 592, 172–175 (2003). [25] Niikura, H. et al. Microlensing constraints on primordial black holes with Subaru/HSC Andromeda observations. Nature Astronomy 3, 524–534 (2019). [26] Sahu, K. C. Stars within the Large Magellanic Cloud as potential lenses for observed microlensing events. Nature 370, 275–276 (1994). [27] Erkal, D. et al. 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Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. 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Limits on the Macho content of the Galactic Halo from the EROS-2 Survey of the Magellanic Clouds. A&A 469, 387–404 (2007). [17] Wyrzykowski, L. et al. The OGLE view of microlensing towards the Magellanic Clouds - IV. OGLE-III SMC data and final conclusions on MACHOs. MNRAS 416, 2949–2961 (2011). [18] Blaineau, T. et al. New limits from microlensing on Galactic black holes in the mass range 10 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT < M < 1000 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT. A&A 664, A106 (2022). [19] Udalski, A. The Optical Gravitational Lensing Experiment. Real Time Data Analysis Systems in the OGLE-III Survey. Acta Astron. 53, 291–305 (2003). [20] Mróz, P. et al. Microlensing optical depth and event rate toward the Large Magellanic Cloud based on 20 years of OGLE observations. submitted (2024). [21] Holtzman, J. A., Afonso, C. & Dolphin, A. 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[29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). 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New limits from microlensing on Galactic black holes in the mass range 10 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT < M < 1000 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT. A&A 664, A106 (2022). [19] Udalski, A. The Optical Gravitational Lensing Experiment. Real Time Data Analysis Systems in the OGLE-III Survey. Acta Astron. 53, 291–305 (2003). [20] Mróz, P. et al. Microlensing optical depth and event rate toward the Large Magellanic Cloud based on 20 years of OGLE observations. submitted (2024). [21] Holtzman, J. A., Afonso, C. & Dolphin, A. The Local Group Stellar Populations Archive from the Hubble Space Telescope WFPC2. ApJS 166, 534–548 (2006). [22] Mróz, P. et al. No large population of unbound or wide-orbit Jupiter-mass planets. Nature 548, 183–186 (2017). [23] Cautun, M. et al. The milky way total mass profile as inferred from Gaia DR2. MNRAS 494, 4291–4313 (2020). [24] Han, C. & Gould, A. Stellar Contribution to the Galactic Bulge Microlensing Optical Depth. ApJ 592, 172–175 (2003). [25] Niikura, H. et al. Microlensing constraints on primordial black holes with Subaru/HSC Andromeda observations. Nature Astronomy 3, 524–534 (2019). [26] Sahu, K. C. Stars within the Large Magellanic Cloud as potential lenses for observed microlensing events. Nature 370, 275–276 (1994). [27] Erkal, D. et al. The total mass of the Large Magellanic Cloud from its perturbation on the Orphan stream. MNRAS 487, 2685–2700 (2019). [28] Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. A&A 678, A208 (2023). [29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. A distance to the Large Magellanic Cloud that is precise to one per cent. Nature 567, 200–203 (2019). [42] Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. An H I Aperture Synthesis Mosaic of the Large Magellanic Cloud. ApJ 503, 674–688 (1998). [44] Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. The dark matter profile of the Milky Way inferred from its circular velocity curve. MNRAS 528, 693–710 (2024). [45] Gaia Collaboration et al. Gaia Data Release 2. 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Microlensing optical depth and event rate toward the Large Magellanic Cloud based on 20 years of OGLE observations. submitted (2024). [21] Holtzman, J. A., Afonso, C. & Dolphin, A. The Local Group Stellar Populations Archive from the Hubble Space Telescope WFPC2. ApJS 166, 534–548 (2006). [22] Mróz, P. et al. No large population of unbound or wide-orbit Jupiter-mass planets. Nature 548, 183–186 (2017). [23] Cautun, M. et al. The milky way total mass profile as inferred from Gaia DR2. MNRAS 494, 4291–4313 (2020). [24] Han, C. & Gould, A. Stellar Contribution to the Galactic Bulge Microlensing Optical Depth. ApJ 592, 172–175 (2003). [25] Niikura, H. et al. Microlensing constraints on primordial black holes with Subaru/HSC Andromeda observations. Nature Astronomy 3, 524–534 (2019). [26] Sahu, K. C. Stars within the Large Magellanic Cloud as potential lenses for observed microlensing events. Nature 370, 275–276 (1994). [27] Erkal, D. et al. The total mass of the Large Magellanic Cloud from its perturbation on the Orphan stream. MNRAS 487, 2685–2700 (2019). [28] Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. A&A 678, A208 (2023). [29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. 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New limits from microlensing on Galactic black holes in the mass range 10 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT < M < 1000 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT. A&A 664, A106 (2022). [19] Udalski, A. The Optical Gravitational Lensing Experiment. Real Time Data Analysis Systems in the OGLE-III Survey. Acta Astron. 53, 291–305 (2003). [20] Mróz, P. et al. Microlensing optical depth and event rate toward the Large Magellanic Cloud based on 20 years of OGLE observations. submitted (2024). [21] Holtzman, J. A., Afonso, C. & Dolphin, A. The Local Group Stellar Populations Archive from the Hubble Space Telescope WFPC2. ApJS 166, 534–548 (2006). [22] Mróz, P. et al. No large population of unbound or wide-orbit Jupiter-mass planets. Nature 548, 183–186 (2017). [23] Cautun, M. et al. The milky way total mass profile as inferred from Gaia DR2. MNRAS 494, 4291–4313 (2020). [24] Han, C. & Gould, A. Stellar Contribution to the Galactic Bulge Microlensing Optical Depth. ApJ 592, 172–175 (2003). [25] Niikura, H. et al. Microlensing constraints on primordial black holes with Subaru/HSC Andromeda observations. Nature Astronomy 3, 524–534 (2019). [26] Sahu, K. C. Stars within the Large Magellanic Cloud as potential lenses for observed microlensing events. Nature 370, 275–276 (1994). [27] Erkal, D. et al. The total mass of the Large Magellanic Cloud from its perturbation on the Orphan stream. MNRAS 487, 2685–2700 (2019). [28] Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. A&A 678, A208 (2023). [29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. A distance to the Large Magellanic Cloud that is precise to one per cent. Nature 567, 200–203 (2019). [42] Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. An H I Aperture Synthesis Mosaic of the Large Magellanic Cloud. ApJ 503, 674–688 (1998). [44] Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. The dark matter profile of the Milky Way inferred from its circular velocity curve. MNRAS 528, 693–710 (2024). [45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021). Blaineau, T. et al. New limits from microlensing on Galactic black holes in the mass range 10 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT < M < 1000 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT. A&A 664, A106 (2022). [19] Udalski, A. The Optical Gravitational Lensing Experiment. Real Time Data Analysis Systems in the OGLE-III Survey. Acta Astron. 53, 291–305 (2003). [20] Mróz, P. et al. Microlensing optical depth and event rate toward the Large Magellanic Cloud based on 20 years of OGLE observations. submitted (2024). [21] Holtzman, J. A., Afonso, C. & Dolphin, A. The Local Group Stellar Populations Archive from the Hubble Space Telescope WFPC2. ApJS 166, 534–548 (2006). [22] Mróz, P. et al. No large population of unbound or wide-orbit Jupiter-mass planets. Nature 548, 183–186 (2017). [23] Cautun, M. et al. The milky way total mass profile as inferred from Gaia DR2. MNRAS 494, 4291–4313 (2020). [24] Han, C. & Gould, A. Stellar Contribution to the Galactic Bulge Microlensing Optical Depth. ApJ 592, 172–175 (2003). [25] Niikura, H. et al. Microlensing constraints on primordial black holes with Subaru/HSC Andromeda observations. Nature Astronomy 3, 524–534 (2019). [26] Sahu, K. C. Stars within the Large Magellanic Cloud as potential lenses for observed microlensing events. Nature 370, 275–276 (1994). [27] Erkal, D. et al. The total mass of the Large Magellanic Cloud from its perturbation on the Orphan stream. MNRAS 487, 2685–2700 (2019). [28] Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. A&A 678, A208 (2023). [29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. 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[37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. A distance to the Large Magellanic Cloud that is precise to one per cent. Nature 567, 200–203 (2019). [42] Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. An H I Aperture Synthesis Mosaic of the Large Magellanic Cloud. ApJ 503, 674–688 (1998). [44] Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. The dark matter profile of the Milky Way inferred from its circular velocity curve. MNRAS 528, 693–710 (2024). [45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021). Udalski, A. The Optical Gravitational Lensing Experiment. Real Time Data Analysis Systems in the OGLE-III Survey. Acta Astron. 53, 291–305 (2003). [20] Mróz, P. et al. Microlensing optical depth and event rate toward the Large Magellanic Cloud based on 20 years of OGLE observations. submitted (2024). [21] Holtzman, J. A., Afonso, C. & Dolphin, A. The Local Group Stellar Populations Archive from the Hubble Space Telescope WFPC2. ApJS 166, 534–548 (2006). [22] Mróz, P. et al. No large population of unbound or wide-orbit Jupiter-mass planets. Nature 548, 183–186 (2017). [23] Cautun, M. et al. The milky way total mass profile as inferred from Gaia DR2. MNRAS 494, 4291–4313 (2020). [24] Han, C. & Gould, A. Stellar Contribution to the Galactic Bulge Microlensing Optical Depth. ApJ 592, 172–175 (2003). [25] Niikura, H. et al. Microlensing constraints on primordial black holes with Subaru/HSC Andromeda observations. Nature Astronomy 3, 524–534 (2019). [26] Sahu, K. C. Stars within the Large Magellanic Cloud as potential lenses for observed microlensing events. Nature 370, 275–276 (1994). [27] Erkal, D. et al. The total mass of the Large Magellanic Cloud from its perturbation on the Orphan stream. MNRAS 487, 2685–2700 (2019). [28] Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. A&A 678, A208 (2023). [29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. A distance to the Large Magellanic Cloud that is precise to one per cent. Nature 567, 200–203 (2019). [42] Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. An H I Aperture Synthesis Mosaic of the Large Magellanic Cloud. ApJ 503, 674–688 (1998). [44] Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. The dark matter profile of the Milky Way inferred from its circular velocity curve. MNRAS 528, 693–710 (2024). [45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021). Mróz, P. et al. Microlensing optical depth and event rate toward the Large Magellanic Cloud based on 20 years of OGLE observations. submitted (2024). [21] Holtzman, J. A., Afonso, C. & Dolphin, A. The Local Group Stellar Populations Archive from the Hubble Space Telescope WFPC2. ApJS 166, 534–548 (2006). [22] Mróz, P. et al. No large population of unbound or wide-orbit Jupiter-mass planets. Nature 548, 183–186 (2017). [23] Cautun, M. et al. The milky way total mass profile as inferred from Gaia DR2. MNRAS 494, 4291–4313 (2020). [24] Han, C. & Gould, A. Stellar Contribution to the Galactic Bulge Microlensing Optical Depth. ApJ 592, 172–175 (2003). [25] Niikura, H. et al. Microlensing constraints on primordial black holes with Subaru/HSC Andromeda observations. Nature Astronomy 3, 524–534 (2019). [26] Sahu, K. C. Stars within the Large Magellanic Cloud as potential lenses for observed microlensing events. Nature 370, 275–276 (1994). [27] Erkal, D. et al. The total mass of the Large Magellanic Cloud from its perturbation on the Orphan stream. MNRAS 487, 2685–2700 (2019). [28] Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. A&A 678, A208 (2023). [29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. A distance to the Large Magellanic Cloud that is precise to one per cent. Nature 567, 200–203 (2019). [42] Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. An H I Aperture Synthesis Mosaic of the Large Magellanic Cloud. ApJ 503, 674–688 (1998). [44] Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. The dark matter profile of the Milky Way inferred from its circular velocity curve. MNRAS 528, 693–710 (2024). [45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021). Holtzman, J. A., Afonso, C. & Dolphin, A. The Local Group Stellar Populations Archive from the Hubble Space Telescope WFPC2. ApJS 166, 534–548 (2006). [22] Mróz, P. et al. No large population of unbound or wide-orbit Jupiter-mass planets. Nature 548, 183–186 (2017). [23] Cautun, M. et al. The milky way total mass profile as inferred from Gaia DR2. MNRAS 494, 4291–4313 (2020). [24] Han, C. & Gould, A. Stellar Contribution to the Galactic Bulge Microlensing Optical Depth. ApJ 592, 172–175 (2003). [25] Niikura, H. et al. Microlensing constraints on primordial black holes with Subaru/HSC Andromeda observations. Nature Astronomy 3, 524–534 (2019). [26] Sahu, K. C. Stars within the Large Magellanic Cloud as potential lenses for observed microlensing events. Nature 370, 275–276 (1994). [27] Erkal, D. et al. The total mass of the Large Magellanic Cloud from its perturbation on the Orphan stream. MNRAS 487, 2685–2700 (2019). [28] Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. A&A 678, A208 (2023). [29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. A distance to the Large Magellanic Cloud that is precise to one per cent. Nature 567, 200–203 (2019). [42] Foreman-Mackey, D., Hogg, D. 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[37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. A distance to the Large Magellanic Cloud that is precise to one per cent. Nature 567, 200–203 (2019). [42] Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. An H I Aperture Synthesis Mosaic of the Large Magellanic Cloud. ApJ 503, 674–688 (1998). [44] Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. 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The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. A distance to the Large Magellanic Cloud that is precise to one per cent. Nature 567, 200–203 (2019). [42] Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. An H I Aperture Synthesis Mosaic of the Large Magellanic Cloud. ApJ 503, 674–688 (1998). [44] Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. The dark matter profile of the Milky Way inferred from its circular velocity curve. MNRAS 528, 693–710 (2024). [45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021). Bird, S. et al. Did LIGO Detect Dark Matter? Phys. Rev. Lett. 116, 201301 (2016). [8] Sasaki, M., Suyama, T., Tanaka, T. & Yokoyama, S. Primordial Black Hole Scenario for the Gravitational-Wave Event GW150914. Phys. Rev. Lett. 117, 061101 (2016). [9] Clesse, S. & García-Bellido, J. The clustering of massive Primordial Black Holes as Dark Matter: Measuring their mass distribution with advanced LIGO. Phys. Dark Universe 15, 142–147 (2017). [10] Carr, B., Clesse, S., García-Bellido, J. & Kühnel, F. Cosmic conundra explained by thermal history and primordial black holes. Phys. Dark Universe 31, 100755 (2021). [11] Jedamzik, K. Consistency of Primordial Black Hole Dark Matter with LIGO/Virgo Merger Rates. Phys. Rev. Lett. 126, 051302 (2021). [12] Escrivà, A., Bagui, E. & Clesse, S. Simulations of PBH formation at the QCD epoch and comparison with the GWTC-3 catalog. J. Cosmology Astropart. Phys 2023, 004 (2023). [13] Udalski, A., Szymański, M. K. & Szymański, G. OGLE-IV: Fourth Phase of the Optical Gravitational Lensing Experiment. Acta Astron. 65, 1–38 (2015). [14] Paczyński, B. Gravitational microlensing by the galactic halo. ApJ 304, 1–5 (1986). [15] Alcock, C. et al. The MACHO Project: Microlensing Results from 5.7 Years of Large Magellanic Cloud Observations. ApJ 542, 281–307 (2000). [16] Tisserand, P. et al. Limits on the Macho content of the Galactic Halo from the EROS-2 Survey of the Magellanic Clouds. A&A 469, 387–404 (2007). [17] Wyrzykowski, L. et al. The OGLE view of microlensing towards the Magellanic Clouds - IV. OGLE-III SMC data and final conclusions on MACHOs. MNRAS 416, 2949–2961 (2011). [18] Blaineau, T. et al. New limits from microlensing on Galactic black holes in the mass range 10 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT < M < 1000 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT. A&A 664, A106 (2022). [19] Udalski, A. The Optical Gravitational Lensing Experiment. Real Time Data Analysis Systems in the OGLE-III Survey. Acta Astron. 53, 291–305 (2003). [20] Mróz, P. et al. Microlensing optical depth and event rate toward the Large Magellanic Cloud based on 20 years of OGLE observations. submitted (2024). [21] Holtzman, J. A., Afonso, C. & Dolphin, A. The Local Group Stellar Populations Archive from the Hubble Space Telescope WFPC2. ApJS 166, 534–548 (2006). [22] Mróz, P. et al. No large population of unbound or wide-orbit Jupiter-mass planets. Nature 548, 183–186 (2017). [23] Cautun, M. et al. The milky way total mass profile as inferred from Gaia DR2. MNRAS 494, 4291–4313 (2020). [24] Han, C. & Gould, A. Stellar Contribution to the Galactic Bulge Microlensing Optical Depth. ApJ 592, 172–175 (2003). [25] Niikura, H. et al. Microlensing constraints on primordial black holes with Subaru/HSC Andromeda observations. Nature Astronomy 3, 524–534 (2019). [26] Sahu, K. C. Stars within the Large Magellanic Cloud as potential lenses for observed microlensing events. Nature 370, 275–276 (1994). [27] Erkal, D. et al. The total mass of the Large Magellanic Cloud from its perturbation on the Orphan stream. MNRAS 487, 2685–2700 (2019). [28] Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. A&A 678, A208 (2023). [29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. A distance to the Large Magellanic Cloud that is precise to one per cent. Nature 567, 200–203 (2019). [42] Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. An H I Aperture Synthesis Mosaic of the Large Magellanic Cloud. ApJ 503, 674–688 (1998). [44] Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. The dark matter profile of the Milky Way inferred from its circular velocity curve. MNRAS 528, 693–710 (2024). [45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021). Sasaki, M., Suyama, T., Tanaka, T. & Yokoyama, S. Primordial Black Hole Scenario for the Gravitational-Wave Event GW150914. Phys. Rev. Lett. 117, 061101 (2016). [9] Clesse, S. & García-Bellido, J. The clustering of massive Primordial Black Holes as Dark Matter: Measuring their mass distribution with advanced LIGO. Phys. Dark Universe 15, 142–147 (2017). [10] Carr, B., Clesse, S., García-Bellido, J. & Kühnel, F. Cosmic conundra explained by thermal history and primordial black holes. Phys. Dark Universe 31, 100755 (2021). [11] Jedamzik, K. Consistency of Primordial Black Hole Dark Matter with LIGO/Virgo Merger Rates. Phys. Rev. Lett. 126, 051302 (2021). [12] Escrivà, A., Bagui, E. & Clesse, S. Simulations of PBH formation at the QCD epoch and comparison with the GWTC-3 catalog. J. Cosmology Astropart. Phys 2023, 004 (2023). [13] Udalski, A., Szymański, M. K. & Szymański, G. OGLE-IV: Fourth Phase of the Optical Gravitational Lensing Experiment. Acta Astron. 65, 1–38 (2015). [14] Paczyński, B. Gravitational microlensing by the galactic halo. ApJ 304, 1–5 (1986). [15] Alcock, C. et al. The MACHO Project: Microlensing Results from 5.7 Years of Large Magellanic Cloud Observations. ApJ 542, 281–307 (2000). [16] Tisserand, P. et al. Limits on the Macho content of the Galactic Halo from the EROS-2 Survey of the Magellanic Clouds. A&A 469, 387–404 (2007). [17] Wyrzykowski, L. et al. The OGLE view of microlensing towards the Magellanic Clouds - IV. OGLE-III SMC data and final conclusions on MACHOs. MNRAS 416, 2949–2961 (2011). [18] Blaineau, T. et al. New limits from microlensing on Galactic black holes in the mass range 10 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT < M < 1000 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT. A&A 664, A106 (2022). [19] Udalski, A. The Optical Gravitational Lensing Experiment. Real Time Data Analysis Systems in the OGLE-III Survey. Acta Astron. 53, 291–305 (2003). [20] Mróz, P. et al. Microlensing optical depth and event rate toward the Large Magellanic Cloud based on 20 years of OGLE observations. submitted (2024). [21] Holtzman, J. A., Afonso, C. & Dolphin, A. The Local Group Stellar Populations Archive from the Hubble Space Telescope WFPC2. ApJS 166, 534–548 (2006). [22] Mróz, P. et al. No large population of unbound or wide-orbit Jupiter-mass planets. Nature 548, 183–186 (2017). [23] Cautun, M. et al. The milky way total mass profile as inferred from Gaia DR2. MNRAS 494, 4291–4313 (2020). [24] Han, C. & Gould, A. Stellar Contribution to the Galactic Bulge Microlensing Optical Depth. ApJ 592, 172–175 (2003). [25] Niikura, H. et al. Microlensing constraints on primordial black holes with Subaru/HSC Andromeda observations. Nature Astronomy 3, 524–534 (2019). [26] Sahu, K. C. Stars within the Large Magellanic Cloud as potential lenses for observed microlensing events. Nature 370, 275–276 (1994). [27] Erkal, D. et al. The total mass of the Large Magellanic Cloud from its perturbation on the Orphan stream. MNRAS 487, 2685–2700 (2019). [28] Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. A&A 678, A208 (2023). [29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. A distance to the Large Magellanic Cloud that is precise to one per cent. Nature 567, 200–203 (2019). [42] Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. An H I Aperture Synthesis Mosaic of the Large Magellanic Cloud. ApJ 503, 674–688 (1998). [44] Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. The dark matter profile of the Milky Way inferred from its circular velocity curve. MNRAS 528, 693–710 (2024). [45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021). Clesse, S. & García-Bellido, J. The clustering of massive Primordial Black Holes as Dark Matter: Measuring their mass distribution with advanced LIGO. Phys. Dark Universe 15, 142–147 (2017). [10] Carr, B., Clesse, S., García-Bellido, J. & Kühnel, F. Cosmic conundra explained by thermal history and primordial black holes. Phys. Dark Universe 31, 100755 (2021). [11] Jedamzik, K. Consistency of Primordial Black Hole Dark Matter with LIGO/Virgo Merger Rates. Phys. Rev. Lett. 126, 051302 (2021). [12] Escrivà, A., Bagui, E. & Clesse, S. Simulations of PBH formation at the QCD epoch and comparison with the GWTC-3 catalog. J. Cosmology Astropart. Phys 2023, 004 (2023). [13] Udalski, A., Szymański, M. K. & Szymański, G. OGLE-IV: Fourth Phase of the Optical Gravitational Lensing Experiment. Acta Astron. 65, 1–38 (2015). [14] Paczyński, B. Gravitational microlensing by the galactic halo. ApJ 304, 1–5 (1986). [15] Alcock, C. et al. The MACHO Project: Microlensing Results from 5.7 Years of Large Magellanic Cloud Observations. ApJ 542, 281–307 (2000). [16] Tisserand, P. et al. Limits on the Macho content of the Galactic Halo from the EROS-2 Survey of the Magellanic Clouds. A&A 469, 387–404 (2007). [17] Wyrzykowski, L. et al. The OGLE view of microlensing towards the Magellanic Clouds - IV. OGLE-III SMC data and final conclusions on MACHOs. MNRAS 416, 2949–2961 (2011). [18] Blaineau, T. et al. New limits from microlensing on Galactic black holes in the mass range 10 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT < M < 1000 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT. A&A 664, A106 (2022). [19] Udalski, A. The Optical Gravitational Lensing Experiment. Real Time Data Analysis Systems in the OGLE-III Survey. Acta Astron. 53, 291–305 (2003). [20] Mróz, P. et al. Microlensing optical depth and event rate toward the Large Magellanic Cloud based on 20 years of OGLE observations. submitted (2024). [21] Holtzman, J. A., Afonso, C. & Dolphin, A. The Local Group Stellar Populations Archive from the Hubble Space Telescope WFPC2. ApJS 166, 534–548 (2006). [22] Mróz, P. et al. No large population of unbound or wide-orbit Jupiter-mass planets. Nature 548, 183–186 (2017). [23] Cautun, M. et al. The milky way total mass profile as inferred from Gaia DR2. MNRAS 494, 4291–4313 (2020). [24] Han, C. & Gould, A. Stellar Contribution to the Galactic Bulge Microlensing Optical Depth. ApJ 592, 172–175 (2003). [25] Niikura, H. et al. Microlensing constraints on primordial black holes with Subaru/HSC Andromeda observations. Nature Astronomy 3, 524–534 (2019). [26] Sahu, K. C. Stars within the Large Magellanic Cloud as potential lenses for observed microlensing events. Nature 370, 275–276 (1994). [27] Erkal, D. et al. The total mass of the Large Magellanic Cloud from its perturbation on the Orphan stream. MNRAS 487, 2685–2700 (2019). [28] Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. A&A 678, A208 (2023). [29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. A distance to the Large Magellanic Cloud that is precise to one per cent. Nature 567, 200–203 (2019). [42] Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. An H I Aperture Synthesis Mosaic of the Large Magellanic Cloud. ApJ 503, 674–688 (1998). [44] Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. The dark matter profile of the Milky Way inferred from its circular velocity curve. MNRAS 528, 693–710 (2024). [45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021). Carr, B., Clesse, S., García-Bellido, J. & Kühnel, F. Cosmic conundra explained by thermal history and primordial black holes. Phys. Dark Universe 31, 100755 (2021). [11] Jedamzik, K. Consistency of Primordial Black Hole Dark Matter with LIGO/Virgo Merger Rates. Phys. Rev. Lett. 126, 051302 (2021). [12] Escrivà, A., Bagui, E. & Clesse, S. Simulations of PBH formation at the QCD epoch and comparison with the GWTC-3 catalog. J. Cosmology Astropart. Phys 2023, 004 (2023). [13] Udalski, A., Szymański, M. K. & Szymański, G. OGLE-IV: Fourth Phase of the Optical Gravitational Lensing Experiment. Acta Astron. 65, 1–38 (2015). [14] Paczyński, B. Gravitational microlensing by the galactic halo. ApJ 304, 1–5 (1986). [15] Alcock, C. et al. The MACHO Project: Microlensing Results from 5.7 Years of Large Magellanic Cloud Observations. ApJ 542, 281–307 (2000). [16] Tisserand, P. et al. Limits on the Macho content of the Galactic Halo from the EROS-2 Survey of the Magellanic Clouds. A&A 469, 387–404 (2007). [17] Wyrzykowski, L. et al. The OGLE view of microlensing towards the Magellanic Clouds - IV. OGLE-III SMC data and final conclusions on MACHOs. MNRAS 416, 2949–2961 (2011). [18] Blaineau, T. et al. New limits from microlensing on Galactic black holes in the mass range 10 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT < M < 1000 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT. A&A 664, A106 (2022). [19] Udalski, A. The Optical Gravitational Lensing Experiment. Real Time Data Analysis Systems in the OGLE-III Survey. Acta Astron. 53, 291–305 (2003). [20] Mróz, P. et al. Microlensing optical depth and event rate toward the Large Magellanic Cloud based on 20 years of OGLE observations. submitted (2024). [21] Holtzman, J. A., Afonso, C. & Dolphin, A. The Local Group Stellar Populations Archive from the Hubble Space Telescope WFPC2. ApJS 166, 534–548 (2006). [22] Mróz, P. et al. No large population of unbound or wide-orbit Jupiter-mass planets. Nature 548, 183–186 (2017). [23] Cautun, M. et al. The milky way total mass profile as inferred from Gaia DR2. MNRAS 494, 4291–4313 (2020). [24] Han, C. & Gould, A. Stellar Contribution to the Galactic Bulge Microlensing Optical Depth. ApJ 592, 172–175 (2003). [25] Niikura, H. et al. Microlensing constraints on primordial black holes with Subaru/HSC Andromeda observations. Nature Astronomy 3, 524–534 (2019). [26] Sahu, K. C. Stars within the Large Magellanic Cloud as potential lenses for observed microlensing events. Nature 370, 275–276 (1994). [27] Erkal, D. et al. The total mass of the Large Magellanic Cloud from its perturbation on the Orphan stream. MNRAS 487, 2685–2700 (2019). [28] Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. A&A 678, A208 (2023). [29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. A distance to the Large Magellanic Cloud that is precise to one per cent. Nature 567, 200–203 (2019). [42] Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. An H I Aperture Synthesis Mosaic of the Large Magellanic Cloud. ApJ 503, 674–688 (1998). [44] Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. The dark matter profile of the Milky Way inferred from its circular velocity curve. MNRAS 528, 693–710 (2024). [45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021). Jedamzik, K. Consistency of Primordial Black Hole Dark Matter with LIGO/Virgo Merger Rates. Phys. Rev. Lett. 126, 051302 (2021). [12] Escrivà, A., Bagui, E. & Clesse, S. Simulations of PBH formation at the QCD epoch and comparison with the GWTC-3 catalog. J. Cosmology Astropart. Phys 2023, 004 (2023). [13] Udalski, A., Szymański, M. K. & Szymański, G. OGLE-IV: Fourth Phase of the Optical Gravitational Lensing Experiment. Acta Astron. 65, 1–38 (2015). [14] Paczyński, B. Gravitational microlensing by the galactic halo. ApJ 304, 1–5 (1986). [15] Alcock, C. et al. The MACHO Project: Microlensing Results from 5.7 Years of Large Magellanic Cloud Observations. ApJ 542, 281–307 (2000). [16] Tisserand, P. et al. Limits on the Macho content of the Galactic Halo from the EROS-2 Survey of the Magellanic Clouds. A&A 469, 387–404 (2007). [17] Wyrzykowski, L. et al. The OGLE view of microlensing towards the Magellanic Clouds - IV. OGLE-III SMC data and final conclusions on MACHOs. MNRAS 416, 2949–2961 (2011). [18] Blaineau, T. et al. New limits from microlensing on Galactic black holes in the mass range 10 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT < M < 1000 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT. A&A 664, A106 (2022). [19] Udalski, A. The Optical Gravitational Lensing Experiment. Real Time Data Analysis Systems in the OGLE-III Survey. Acta Astron. 53, 291–305 (2003). [20] Mróz, P. et al. Microlensing optical depth and event rate toward the Large Magellanic Cloud based on 20 years of OGLE observations. submitted (2024). [21] Holtzman, J. A., Afonso, C. & Dolphin, A. The Local Group Stellar Populations Archive from the Hubble Space Telescope WFPC2. ApJS 166, 534–548 (2006). [22] Mróz, P. et al. No large population of unbound or wide-orbit Jupiter-mass planets. Nature 548, 183–186 (2017). [23] Cautun, M. et al. The milky way total mass profile as inferred from Gaia DR2. MNRAS 494, 4291–4313 (2020). [24] Han, C. & Gould, A. Stellar Contribution to the Galactic Bulge Microlensing Optical Depth. ApJ 592, 172–175 (2003). [25] Niikura, H. et al. Microlensing constraints on primordial black holes with Subaru/HSC Andromeda observations. Nature Astronomy 3, 524–534 (2019). [26] Sahu, K. C. Stars within the Large Magellanic Cloud as potential lenses for observed microlensing events. Nature 370, 275–276 (1994). [27] Erkal, D. et al. The total mass of the Large Magellanic Cloud from its perturbation on the Orphan stream. MNRAS 487, 2685–2700 (2019). [28] Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. A&A 678, A208 (2023). [29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. A distance to the Large Magellanic Cloud that is precise to one per cent. Nature 567, 200–203 (2019). [42] Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. An H I Aperture Synthesis Mosaic of the Large Magellanic Cloud. ApJ 503, 674–688 (1998). [44] Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. The dark matter profile of the Milky Way inferred from its circular velocity curve. MNRAS 528, 693–710 (2024). [45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021). Escrivà, A., Bagui, E. & Clesse, S. Simulations of PBH formation at the QCD epoch and comparison with the GWTC-3 catalog. J. Cosmology Astropart. Phys 2023, 004 (2023). [13] Udalski, A., Szymański, M. K. & Szymański, G. OGLE-IV: Fourth Phase of the Optical Gravitational Lensing Experiment. Acta Astron. 65, 1–38 (2015). [14] Paczyński, B. Gravitational microlensing by the galactic halo. ApJ 304, 1–5 (1986). [15] Alcock, C. et al. The MACHO Project: Microlensing Results from 5.7 Years of Large Magellanic Cloud Observations. ApJ 542, 281–307 (2000). [16] Tisserand, P. et al. Limits on the Macho content of the Galactic Halo from the EROS-2 Survey of the Magellanic Clouds. A&A 469, 387–404 (2007). [17] Wyrzykowski, L. et al. The OGLE view of microlensing towards the Magellanic Clouds - IV. OGLE-III SMC data and final conclusions on MACHOs. MNRAS 416, 2949–2961 (2011). [18] Blaineau, T. et al. New limits from microlensing on Galactic black holes in the mass range 10 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT < M < 1000 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT. A&A 664, A106 (2022). [19] Udalski, A. The Optical Gravitational Lensing Experiment. Real Time Data Analysis Systems in the OGLE-III Survey. Acta Astron. 53, 291–305 (2003). [20] Mróz, P. et al. Microlensing optical depth and event rate toward the Large Magellanic Cloud based on 20 years of OGLE observations. submitted (2024). [21] Holtzman, J. A., Afonso, C. & Dolphin, A. The Local Group Stellar Populations Archive from the Hubble Space Telescope WFPC2. ApJS 166, 534–548 (2006). [22] Mróz, P. et al. No large population of unbound or wide-orbit Jupiter-mass planets. Nature 548, 183–186 (2017). [23] Cautun, M. et al. The milky way total mass profile as inferred from Gaia DR2. MNRAS 494, 4291–4313 (2020). [24] Han, C. & Gould, A. Stellar Contribution to the Galactic Bulge Microlensing Optical Depth. ApJ 592, 172–175 (2003). [25] Niikura, H. et al. Microlensing constraints on primordial black holes with Subaru/HSC Andromeda observations. Nature Astronomy 3, 524–534 (2019). [26] Sahu, K. C. Stars within the Large Magellanic Cloud as potential lenses for observed microlensing events. Nature 370, 275–276 (1994). [27] Erkal, D. et al. The total mass of the Large Magellanic Cloud from its perturbation on the Orphan stream. MNRAS 487, 2685–2700 (2019). [28] Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. A&A 678, A208 (2023). [29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. A distance to the Large Magellanic Cloud that is precise to one per cent. Nature 567, 200–203 (2019). [42] Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. An H I Aperture Synthesis Mosaic of the Large Magellanic Cloud. ApJ 503, 674–688 (1998). [44] Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. The dark matter profile of the Milky Way inferred from its circular velocity curve. MNRAS 528, 693–710 (2024). [45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021). Udalski, A., Szymański, M. K. & Szymański, G. OGLE-IV: Fourth Phase of the Optical Gravitational Lensing Experiment. Acta Astron. 65, 1–38 (2015). [14] Paczyński, B. Gravitational microlensing by the galactic halo. ApJ 304, 1–5 (1986). [15] Alcock, C. et al. The MACHO Project: Microlensing Results from 5.7 Years of Large Magellanic Cloud Observations. ApJ 542, 281–307 (2000). [16] Tisserand, P. et al. Limits on the Macho content of the Galactic Halo from the EROS-2 Survey of the Magellanic Clouds. A&A 469, 387–404 (2007). [17] Wyrzykowski, L. et al. The OGLE view of microlensing towards the Magellanic Clouds - IV. OGLE-III SMC data and final conclusions on MACHOs. MNRAS 416, 2949–2961 (2011). [18] Blaineau, T. et al. New limits from microlensing on Galactic black holes in the mass range 10 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT < M < 1000 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT. A&A 664, A106 (2022). [19] Udalski, A. The Optical Gravitational Lensing Experiment. Real Time Data Analysis Systems in the OGLE-III Survey. Acta Astron. 53, 291–305 (2003). [20] Mróz, P. et al. Microlensing optical depth and event rate toward the Large Magellanic Cloud based on 20 years of OGLE observations. submitted (2024). [21] Holtzman, J. A., Afonso, C. & Dolphin, A. The Local Group Stellar Populations Archive from the Hubble Space Telescope WFPC2. ApJS 166, 534–548 (2006). [22] Mróz, P. et al. No large population of unbound or wide-orbit Jupiter-mass planets. Nature 548, 183–186 (2017). [23] Cautun, M. et al. The milky way total mass profile as inferred from Gaia DR2. MNRAS 494, 4291–4313 (2020). [24] Han, C. & Gould, A. Stellar Contribution to the Galactic Bulge Microlensing Optical Depth. ApJ 592, 172–175 (2003). [25] Niikura, H. et al. Microlensing constraints on primordial black holes with Subaru/HSC Andromeda observations. Nature Astronomy 3, 524–534 (2019). [26] Sahu, K. C. Stars within the Large Magellanic Cloud as potential lenses for observed microlensing events. Nature 370, 275–276 (1994). [27] Erkal, D. et al. The total mass of the Large Magellanic Cloud from its perturbation on the Orphan stream. MNRAS 487, 2685–2700 (2019). [28] Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. A&A 678, A208 (2023). [29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. A distance to the Large Magellanic Cloud that is precise to one per cent. Nature 567, 200–203 (2019). [42] Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. An H I Aperture Synthesis Mosaic of the Large Magellanic Cloud. ApJ 503, 674–688 (1998). [44] Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. The dark matter profile of the Milky Way inferred from its circular velocity curve. MNRAS 528, 693–710 (2024). [45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021). Paczyński, B. Gravitational microlensing by the galactic halo. ApJ 304, 1–5 (1986). [15] Alcock, C. et al. The MACHO Project: Microlensing Results from 5.7 Years of Large Magellanic Cloud Observations. ApJ 542, 281–307 (2000). [16] Tisserand, P. et al. Limits on the Macho content of the Galactic Halo from the EROS-2 Survey of the Magellanic Clouds. A&A 469, 387–404 (2007). [17] Wyrzykowski, L. et al. The OGLE view of microlensing towards the Magellanic Clouds - IV. OGLE-III SMC data and final conclusions on MACHOs. MNRAS 416, 2949–2961 (2011). [18] Blaineau, T. et al. New limits from microlensing on Galactic black holes in the mass range 10 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT < M < 1000 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT. A&A 664, A106 (2022). [19] Udalski, A. The Optical Gravitational Lensing Experiment. Real Time Data Analysis Systems in the OGLE-III Survey. Acta Astron. 53, 291–305 (2003). [20] Mróz, P. et al. Microlensing optical depth and event rate toward the Large Magellanic Cloud based on 20 years of OGLE observations. submitted (2024). [21] Holtzman, J. A., Afonso, C. & Dolphin, A. The Local Group Stellar Populations Archive from the Hubble Space Telescope WFPC2. ApJS 166, 534–548 (2006). [22] Mróz, P. et al. No large population of unbound or wide-orbit Jupiter-mass planets. Nature 548, 183–186 (2017). [23] Cautun, M. et al. The milky way total mass profile as inferred from Gaia DR2. MNRAS 494, 4291–4313 (2020). [24] Han, C. & Gould, A. Stellar Contribution to the Galactic Bulge Microlensing Optical Depth. ApJ 592, 172–175 (2003). [25] Niikura, H. et al. Microlensing constraints on primordial black holes with Subaru/HSC Andromeda observations. Nature Astronomy 3, 524–534 (2019). [26] Sahu, K. C. Stars within the Large Magellanic Cloud as potential lenses for observed microlensing events. Nature 370, 275–276 (1994). [27] Erkal, D. et al. The total mass of the Large Magellanic Cloud from its perturbation on the Orphan stream. MNRAS 487, 2685–2700 (2019). [28] Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. A&A 678, A208 (2023). [29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. A distance to the Large Magellanic Cloud that is precise to one per cent. Nature 567, 200–203 (2019). [42] Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. An H I Aperture Synthesis Mosaic of the Large Magellanic Cloud. ApJ 503, 674–688 (1998). [44] Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. The dark matter profile of the Milky Way inferred from its circular velocity curve. MNRAS 528, 693–710 (2024). [45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021). Alcock, C. et al. The MACHO Project: Microlensing Results from 5.7 Years of Large Magellanic Cloud Observations. ApJ 542, 281–307 (2000). [16] Tisserand, P. et al. Limits on the Macho content of the Galactic Halo from the EROS-2 Survey of the Magellanic Clouds. A&A 469, 387–404 (2007). [17] Wyrzykowski, L. et al. The OGLE view of microlensing towards the Magellanic Clouds - IV. OGLE-III SMC data and final conclusions on MACHOs. MNRAS 416, 2949–2961 (2011). [18] Blaineau, T. et al. New limits from microlensing on Galactic black holes in the mass range 10 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT < M < 1000 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT. A&A 664, A106 (2022). [19] Udalski, A. The Optical Gravitational Lensing Experiment. Real Time Data Analysis Systems in the OGLE-III Survey. Acta Astron. 53, 291–305 (2003). [20] Mróz, P. et al. Microlensing optical depth and event rate toward the Large Magellanic Cloud based on 20 years of OGLE observations. submitted (2024). [21] Holtzman, J. A., Afonso, C. & Dolphin, A. The Local Group Stellar Populations Archive from the Hubble Space Telescope WFPC2. ApJS 166, 534–548 (2006). [22] Mróz, P. et al. No large population of unbound or wide-orbit Jupiter-mass planets. Nature 548, 183–186 (2017). [23] Cautun, M. et al. The milky way total mass profile as inferred from Gaia DR2. MNRAS 494, 4291–4313 (2020). [24] Han, C. & Gould, A. Stellar Contribution to the Galactic Bulge Microlensing Optical Depth. ApJ 592, 172–175 (2003). [25] Niikura, H. et al. Microlensing constraints on primordial black holes with Subaru/HSC Andromeda observations. Nature Astronomy 3, 524–534 (2019). [26] Sahu, K. C. Stars within the Large Magellanic Cloud as potential lenses for observed microlensing events. Nature 370, 275–276 (1994). [27] Erkal, D. et al. The total mass of the Large Magellanic Cloud from its perturbation on the Orphan stream. MNRAS 487, 2685–2700 (2019). [28] Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. A&A 678, A208 (2023). [29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. A distance to the Large Magellanic Cloud that is precise to one per cent. Nature 567, 200–203 (2019). [42] Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. An H I Aperture Synthesis Mosaic of the Large Magellanic Cloud. ApJ 503, 674–688 (1998). [44] Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. The dark matter profile of the Milky Way inferred from its circular velocity curve. MNRAS 528, 693–710 (2024). [45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021). Tisserand, P. et al. Limits on the Macho content of the Galactic Halo from the EROS-2 Survey of the Magellanic Clouds. A&A 469, 387–404 (2007). [17] Wyrzykowski, L. et al. The OGLE view of microlensing towards the Magellanic Clouds - IV. OGLE-III SMC data and final conclusions on MACHOs. MNRAS 416, 2949–2961 (2011). [18] Blaineau, T. et al. New limits from microlensing on Galactic black holes in the mass range 10 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT < M < 1000 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT. A&A 664, A106 (2022). [19] Udalski, A. The Optical Gravitational Lensing Experiment. Real Time Data Analysis Systems in the OGLE-III Survey. Acta Astron. 53, 291–305 (2003). [20] Mróz, P. et al. Microlensing optical depth and event rate toward the Large Magellanic Cloud based on 20 years of OGLE observations. submitted (2024). [21] Holtzman, J. A., Afonso, C. & Dolphin, A. The Local Group Stellar Populations Archive from the Hubble Space Telescope WFPC2. ApJS 166, 534–548 (2006). [22] Mróz, P. et al. No large population of unbound or wide-orbit Jupiter-mass planets. Nature 548, 183–186 (2017). [23] Cautun, M. et al. The milky way total mass profile as inferred from Gaia DR2. MNRAS 494, 4291–4313 (2020). [24] Han, C. & Gould, A. Stellar Contribution to the Galactic Bulge Microlensing Optical Depth. ApJ 592, 172–175 (2003). [25] Niikura, H. et al. Microlensing constraints on primordial black holes with Subaru/HSC Andromeda observations. Nature Astronomy 3, 524–534 (2019). [26] Sahu, K. C. Stars within the Large Magellanic Cloud as potential lenses for observed microlensing events. Nature 370, 275–276 (1994). [27] Erkal, D. et al. The total mass of the Large Magellanic Cloud from its perturbation on the Orphan stream. MNRAS 487, 2685–2700 (2019). [28] Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. A&A 678, A208 (2023). [29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. A distance to the Large Magellanic Cloud that is precise to one per cent. Nature 567, 200–203 (2019). [42] Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. An H I Aperture Synthesis Mosaic of the Large Magellanic Cloud. ApJ 503, 674–688 (1998). [44] Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. The dark matter profile of the Milky Way inferred from its circular velocity curve. MNRAS 528, 693–710 (2024). [45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021). Wyrzykowski, L. et al. The OGLE view of microlensing towards the Magellanic Clouds - IV. OGLE-III SMC data and final conclusions on MACHOs. MNRAS 416, 2949–2961 (2011). [18] Blaineau, T. et al. New limits from microlensing on Galactic black holes in the mass range 10 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT < M < 1000 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT. A&A 664, A106 (2022). [19] Udalski, A. The Optical Gravitational Lensing Experiment. Real Time Data Analysis Systems in the OGLE-III Survey. Acta Astron. 53, 291–305 (2003). [20] Mróz, P. et al. Microlensing optical depth and event rate toward the Large Magellanic Cloud based on 20 years of OGLE observations. submitted (2024). [21] Holtzman, J. A., Afonso, C. & Dolphin, A. The Local Group Stellar Populations Archive from the Hubble Space Telescope WFPC2. ApJS 166, 534–548 (2006). [22] Mróz, P. et al. No large population of unbound or wide-orbit Jupiter-mass planets. Nature 548, 183–186 (2017). [23] Cautun, M. et al. The milky way total mass profile as inferred from Gaia DR2. MNRAS 494, 4291–4313 (2020). [24] Han, C. & Gould, A. Stellar Contribution to the Galactic Bulge Microlensing Optical Depth. ApJ 592, 172–175 (2003). [25] Niikura, H. et al. Microlensing constraints on primordial black holes with Subaru/HSC Andromeda observations. Nature Astronomy 3, 524–534 (2019). [26] Sahu, K. C. Stars within the Large Magellanic Cloud as potential lenses for observed microlensing events. Nature 370, 275–276 (1994). [27] Erkal, D. et al. The total mass of the Large Magellanic Cloud from its perturbation on the Orphan stream. MNRAS 487, 2685–2700 (2019). [28] Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. A&A 678, A208 (2023). [29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. A distance to the Large Magellanic Cloud that is precise to one per cent. Nature 567, 200–203 (2019). [42] Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. An H I Aperture Synthesis Mosaic of the Large Magellanic Cloud. ApJ 503, 674–688 (1998). [44] Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. The dark matter profile of the Milky Way inferred from its circular velocity curve. MNRAS 528, 693–710 (2024). [45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021). Blaineau, T. et al. New limits from microlensing on Galactic black holes in the mass range 10 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT < M < 1000 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT. A&A 664, A106 (2022). [19] Udalski, A. The Optical Gravitational Lensing Experiment. Real Time Data Analysis Systems in the OGLE-III Survey. Acta Astron. 53, 291–305 (2003). [20] Mróz, P. et al. Microlensing optical depth and event rate toward the Large Magellanic Cloud based on 20 years of OGLE observations. submitted (2024). [21] Holtzman, J. A., Afonso, C. & Dolphin, A. The Local Group Stellar Populations Archive from the Hubble Space Telescope WFPC2. ApJS 166, 534–548 (2006). [22] Mróz, P. et al. No large population of unbound or wide-orbit Jupiter-mass planets. Nature 548, 183–186 (2017). [23] Cautun, M. et al. The milky way total mass profile as inferred from Gaia DR2. MNRAS 494, 4291–4313 (2020). [24] Han, C. & Gould, A. Stellar Contribution to the Galactic Bulge Microlensing Optical Depth. ApJ 592, 172–175 (2003). [25] Niikura, H. et al. Microlensing constraints on primordial black holes with Subaru/HSC Andromeda observations. Nature Astronomy 3, 524–534 (2019). [26] Sahu, K. C. Stars within the Large Magellanic Cloud as potential lenses for observed microlensing events. Nature 370, 275–276 (1994). [27] Erkal, D. et al. The total mass of the Large Magellanic Cloud from its perturbation on the Orphan stream. MNRAS 487, 2685–2700 (2019). [28] Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. A&A 678, A208 (2023). [29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. A distance to the Large Magellanic Cloud that is precise to one per cent. Nature 567, 200–203 (2019). [42] Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. An H I Aperture Synthesis Mosaic of the Large Magellanic Cloud. ApJ 503, 674–688 (1998). [44] Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. The dark matter profile of the Milky Way inferred from its circular velocity curve. MNRAS 528, 693–710 (2024). [45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021). Udalski, A. The Optical Gravitational Lensing Experiment. Real Time Data Analysis Systems in the OGLE-III Survey. Acta Astron. 53, 291–305 (2003). [20] Mróz, P. et al. Microlensing optical depth and event rate toward the Large Magellanic Cloud based on 20 years of OGLE observations. submitted (2024). [21] Holtzman, J. A., Afonso, C. & Dolphin, A. The Local Group Stellar Populations Archive from the Hubble Space Telescope WFPC2. ApJS 166, 534–548 (2006). [22] Mróz, P. et al. No large population of unbound or wide-orbit Jupiter-mass planets. Nature 548, 183–186 (2017). [23] Cautun, M. et al. The milky way total mass profile as inferred from Gaia DR2. MNRAS 494, 4291–4313 (2020). [24] Han, C. & Gould, A. Stellar Contribution to the Galactic Bulge Microlensing Optical Depth. ApJ 592, 172–175 (2003). [25] Niikura, H. et al. Microlensing constraints on primordial black holes with Subaru/HSC Andromeda observations. Nature Astronomy 3, 524–534 (2019). [26] Sahu, K. C. Stars within the Large Magellanic Cloud as potential lenses for observed microlensing events. Nature 370, 275–276 (1994). [27] Erkal, D. et al. The total mass of the Large Magellanic Cloud from its perturbation on the Orphan stream. MNRAS 487, 2685–2700 (2019). [28] Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. A&A 678, A208 (2023). [29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. A distance to the Large Magellanic Cloud that is precise to one per cent. Nature 567, 200–203 (2019). [42] Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. An H I Aperture Synthesis Mosaic of the Large Magellanic Cloud. ApJ 503, 674–688 (1998). [44] Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. The dark matter profile of the Milky Way inferred from its circular velocity curve. MNRAS 528, 693–710 (2024). [45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021). Mróz, P. et al. Microlensing optical depth and event rate toward the Large Magellanic Cloud based on 20 years of OGLE observations. submitted (2024). [21] Holtzman, J. A., Afonso, C. & Dolphin, A. The Local Group Stellar Populations Archive from the Hubble Space Telescope WFPC2. ApJS 166, 534–548 (2006). [22] Mróz, P. et al. No large population of unbound or wide-orbit Jupiter-mass planets. Nature 548, 183–186 (2017). [23] Cautun, M. et al. The milky way total mass profile as inferred from Gaia DR2. MNRAS 494, 4291–4313 (2020). [24] Han, C. & Gould, A. Stellar Contribution to the Galactic Bulge Microlensing Optical Depth. ApJ 592, 172–175 (2003). [25] Niikura, H. et al. Microlensing constraints on primordial black holes with Subaru/HSC Andromeda observations. Nature Astronomy 3, 524–534 (2019). [26] Sahu, K. C. Stars within the Large Magellanic Cloud as potential lenses for observed microlensing events. Nature 370, 275–276 (1994). [27] Erkal, D. et al. The total mass of the Large Magellanic Cloud from its perturbation on the Orphan stream. MNRAS 487, 2685–2700 (2019). [28] Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. A&A 678, A208 (2023). [29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. 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[45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021). Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. A&A 678, A208 (2023). [29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. 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OGLE-IV: Fourth Phase of the Optical Gravitational Lensing Experiment. Acta Astron. 65, 1–38 (2015). [14] Paczyński, B. Gravitational microlensing by the galactic halo. ApJ 304, 1–5 (1986). [15] Alcock, C. et al. The MACHO Project: Microlensing Results from 5.7 Years of Large Magellanic Cloud Observations. ApJ 542, 281–307 (2000). [16] Tisserand, P. et al. Limits on the Macho content of the Galactic Halo from the EROS-2 Survey of the Magellanic Clouds. A&A 469, 387–404 (2007). [17] Wyrzykowski, L. et al. The OGLE view of microlensing towards the Magellanic Clouds - IV. OGLE-III SMC data and final conclusions on MACHOs. MNRAS 416, 2949–2961 (2011). [18] Blaineau, T. et al. New limits from microlensing on Galactic black holes in the mass range 10 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT < M < 1000 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT. A&A 664, A106 (2022). [19] Udalski, A. The Optical Gravitational Lensing Experiment. Real Time Data Analysis Systems in the OGLE-III Survey. Acta Astron. 53, 291–305 (2003). [20] Mróz, P. et al. Microlensing optical depth and event rate toward the Large Magellanic Cloud based on 20 years of OGLE observations. submitted (2024). [21] Holtzman, J. A., Afonso, C. & Dolphin, A. The Local Group Stellar Populations Archive from the Hubble Space Telescope WFPC2. ApJS 166, 534–548 (2006). [22] Mróz, P. et al. No large population of unbound or wide-orbit Jupiter-mass planets. Nature 548, 183–186 (2017). [23] Cautun, M. et al. The milky way total mass profile as inferred from Gaia DR2. MNRAS 494, 4291–4313 (2020). [24] Han, C. & Gould, A. Stellar Contribution to the Galactic Bulge Microlensing Optical Depth. ApJ 592, 172–175 (2003). [25] Niikura, H. et al. Microlensing constraints on primordial black holes with Subaru/HSC Andromeda observations. Nature Astronomy 3, 524–534 (2019). [26] Sahu, K. C. Stars within the Large Magellanic Cloud as potential lenses for observed microlensing events. Nature 370, 275–276 (1994). [27] Erkal, D. et al. The total mass of the Large Magellanic Cloud from its perturbation on the Orphan stream. MNRAS 487, 2685–2700 (2019). [28] Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. A&A 678, A208 (2023). [29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. A distance to the Large Magellanic Cloud that is precise to one per cent. Nature 567, 200–203 (2019). [42] Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. An H I Aperture Synthesis Mosaic of the Large Magellanic Cloud. ApJ 503, 674–688 (1998). [44] Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. The dark matter profile of the Milky Way inferred from its circular velocity curve. MNRAS 528, 693–710 (2024). [45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021). Sasaki, M., Suyama, T., Tanaka, T. & Yokoyama, S. Primordial Black Hole Scenario for the Gravitational-Wave Event GW150914. Phys. Rev. Lett. 117, 061101 (2016). [9] Clesse, S. & García-Bellido, J. The clustering of massive Primordial Black Holes as Dark Matter: Measuring their mass distribution with advanced LIGO. Phys. Dark Universe 15, 142–147 (2017). [10] Carr, B., Clesse, S., García-Bellido, J. & Kühnel, F. Cosmic conundra explained by thermal history and primordial black holes. Phys. Dark Universe 31, 100755 (2021). [11] Jedamzik, K. Consistency of Primordial Black Hole Dark Matter with LIGO/Virgo Merger Rates. Phys. Rev. Lett. 126, 051302 (2021). [12] Escrivà, A., Bagui, E. & Clesse, S. Simulations of PBH formation at the QCD epoch and comparison with the GWTC-3 catalog. J. Cosmology Astropart. Phys 2023, 004 (2023). [13] Udalski, A., Szymański, M. K. & Szymański, G. OGLE-IV: Fourth Phase of the Optical Gravitational Lensing Experiment. Acta Astron. 65, 1–38 (2015). [14] Paczyński, B. Gravitational microlensing by the galactic halo. ApJ 304, 1–5 (1986). [15] Alcock, C. et al. The MACHO Project: Microlensing Results from 5.7 Years of Large Magellanic Cloud Observations. ApJ 542, 281–307 (2000). [16] Tisserand, P. et al. Limits on the Macho content of the Galactic Halo from the EROS-2 Survey of the Magellanic Clouds. A&A 469, 387–404 (2007). [17] Wyrzykowski, L. et al. The OGLE view of microlensing towards the Magellanic Clouds - IV. OGLE-III SMC data and final conclusions on MACHOs. MNRAS 416, 2949–2961 (2011). [18] Blaineau, T. et al. New limits from microlensing on Galactic black holes in the mass range 10 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT < M < 1000 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT. A&A 664, A106 (2022). [19] Udalski, A. The Optical Gravitational Lensing Experiment. Real Time Data Analysis Systems in the OGLE-III Survey. Acta Astron. 53, 291–305 (2003). [20] Mróz, P. et al. Microlensing optical depth and event rate toward the Large Magellanic Cloud based on 20 years of OGLE observations. submitted (2024). [21] Holtzman, J. A., Afonso, C. & Dolphin, A. The Local Group Stellar Populations Archive from the Hubble Space Telescope WFPC2. ApJS 166, 534–548 (2006). [22] Mróz, P. et al. No large population of unbound or wide-orbit Jupiter-mass planets. Nature 548, 183–186 (2017). [23] Cautun, M. et al. The milky way total mass profile as inferred from Gaia DR2. MNRAS 494, 4291–4313 (2020). [24] Han, C. & Gould, A. Stellar Contribution to the Galactic Bulge Microlensing Optical Depth. ApJ 592, 172–175 (2003). [25] Niikura, H. et al. Microlensing constraints on primordial black holes with Subaru/HSC Andromeda observations. Nature Astronomy 3, 524–534 (2019). [26] Sahu, K. C. Stars within the Large Magellanic Cloud as potential lenses for observed microlensing events. Nature 370, 275–276 (1994). [27] Erkal, D. et al. The total mass of the Large Magellanic Cloud from its perturbation on the Orphan stream. MNRAS 487, 2685–2700 (2019). [28] Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. A&A 678, A208 (2023). [29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. A distance to the Large Magellanic Cloud that is precise to one per cent. Nature 567, 200–203 (2019). [42] Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. An H I Aperture Synthesis Mosaic of the Large Magellanic Cloud. ApJ 503, 674–688 (1998). [44] Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. The dark matter profile of the Milky Way inferred from its circular velocity curve. MNRAS 528, 693–710 (2024). [45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021). Clesse, S. & García-Bellido, J. The clustering of massive Primordial Black Holes as Dark Matter: Measuring their mass distribution with advanced LIGO. Phys. Dark Universe 15, 142–147 (2017). [10] Carr, B., Clesse, S., García-Bellido, J. & Kühnel, F. Cosmic conundra explained by thermal history and primordial black holes. Phys. Dark Universe 31, 100755 (2021). [11] Jedamzik, K. Consistency of Primordial Black Hole Dark Matter with LIGO/Virgo Merger Rates. Phys. Rev. Lett. 126, 051302 (2021). [12] Escrivà, A., Bagui, E. & Clesse, S. Simulations of PBH formation at the QCD epoch and comparison with the GWTC-3 catalog. J. Cosmology Astropart. Phys 2023, 004 (2023). [13] Udalski, A., Szymański, M. K. & Szymański, G. OGLE-IV: Fourth Phase of the Optical Gravitational Lensing Experiment. Acta Astron. 65, 1–38 (2015). [14] Paczyński, B. Gravitational microlensing by the galactic halo. ApJ 304, 1–5 (1986). [15] Alcock, C. et al. The MACHO Project: Microlensing Results from 5.7 Years of Large Magellanic Cloud Observations. ApJ 542, 281–307 (2000). [16] Tisserand, P. et al. Limits on the Macho content of the Galactic Halo from the EROS-2 Survey of the Magellanic Clouds. A&A 469, 387–404 (2007). [17] Wyrzykowski, L. et al. The OGLE view of microlensing towards the Magellanic Clouds - IV. OGLE-III SMC data and final conclusions on MACHOs. MNRAS 416, 2949–2961 (2011). [18] Blaineau, T. et al. New limits from microlensing on Galactic black holes in the mass range 10 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT < M < 1000 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT. A&A 664, A106 (2022). [19] Udalski, A. The Optical Gravitational Lensing Experiment. Real Time Data Analysis Systems in the OGLE-III Survey. Acta Astron. 53, 291–305 (2003). [20] Mróz, P. et al. Microlensing optical depth and event rate toward the Large Magellanic Cloud based on 20 years of OGLE observations. submitted (2024). [21] Holtzman, J. A., Afonso, C. & Dolphin, A. The Local Group Stellar Populations Archive from the Hubble Space Telescope WFPC2. ApJS 166, 534–548 (2006). [22] Mróz, P. et al. No large population of unbound or wide-orbit Jupiter-mass planets. Nature 548, 183–186 (2017). [23] Cautun, M. et al. The milky way total mass profile as inferred from Gaia DR2. MNRAS 494, 4291–4313 (2020). [24] Han, C. & Gould, A. Stellar Contribution to the Galactic Bulge Microlensing Optical Depth. ApJ 592, 172–175 (2003). [25] Niikura, H. et al. Microlensing constraints on primordial black holes with Subaru/HSC Andromeda observations. Nature Astronomy 3, 524–534 (2019). [26] Sahu, K. C. Stars within the Large Magellanic Cloud as potential lenses for observed microlensing events. Nature 370, 275–276 (1994). [27] Erkal, D. et al. The total mass of the Large Magellanic Cloud from its perturbation on the Orphan stream. MNRAS 487, 2685–2700 (2019). [28] Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. A&A 678, A208 (2023). [29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. A distance to the Large Magellanic Cloud that is precise to one per cent. Nature 567, 200–203 (2019). [42] Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. An H I Aperture Synthesis Mosaic of the Large Magellanic Cloud. ApJ 503, 674–688 (1998). [44] Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. The dark matter profile of the Milky Way inferred from its circular velocity curve. MNRAS 528, 693–710 (2024). [45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021). Carr, B., Clesse, S., García-Bellido, J. & Kühnel, F. Cosmic conundra explained by thermal history and primordial black holes. Phys. Dark Universe 31, 100755 (2021). [11] Jedamzik, K. Consistency of Primordial Black Hole Dark Matter with LIGO/Virgo Merger Rates. Phys. Rev. Lett. 126, 051302 (2021). [12] Escrivà, A., Bagui, E. & Clesse, S. Simulations of PBH formation at the QCD epoch and comparison with the GWTC-3 catalog. J. Cosmology Astropart. Phys 2023, 004 (2023). [13] Udalski, A., Szymański, M. K. & Szymański, G. OGLE-IV: Fourth Phase of the Optical Gravitational Lensing Experiment. Acta Astron. 65, 1–38 (2015). [14] Paczyński, B. Gravitational microlensing by the galactic halo. ApJ 304, 1–5 (1986). [15] Alcock, C. et al. The MACHO Project: Microlensing Results from 5.7 Years of Large Magellanic Cloud Observations. ApJ 542, 281–307 (2000). [16] Tisserand, P. et al. Limits on the Macho content of the Galactic Halo from the EROS-2 Survey of the Magellanic Clouds. A&A 469, 387–404 (2007). [17] Wyrzykowski, L. et al. The OGLE view of microlensing towards the Magellanic Clouds - IV. OGLE-III SMC data and final conclusions on MACHOs. MNRAS 416, 2949–2961 (2011). [18] Blaineau, T. et al. New limits from microlensing on Galactic black holes in the mass range 10 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT < M < 1000 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT. A&A 664, A106 (2022). [19] Udalski, A. The Optical Gravitational Lensing Experiment. Real Time Data Analysis Systems in the OGLE-III Survey. Acta Astron. 53, 291–305 (2003). [20] Mróz, P. et al. Microlensing optical depth and event rate toward the Large Magellanic Cloud based on 20 years of OGLE observations. submitted (2024). [21] Holtzman, J. A., Afonso, C. & Dolphin, A. The Local Group Stellar Populations Archive from the Hubble Space Telescope WFPC2. ApJS 166, 534–548 (2006). [22] Mróz, P. et al. No large population of unbound or wide-orbit Jupiter-mass planets. Nature 548, 183–186 (2017). [23] Cautun, M. et al. The milky way total mass profile as inferred from Gaia DR2. MNRAS 494, 4291–4313 (2020). [24] Han, C. & Gould, A. Stellar Contribution to the Galactic Bulge Microlensing Optical Depth. ApJ 592, 172–175 (2003). [25] Niikura, H. et al. Microlensing constraints on primordial black holes with Subaru/HSC Andromeda observations. Nature Astronomy 3, 524–534 (2019). [26] Sahu, K. C. Stars within the Large Magellanic Cloud as potential lenses for observed microlensing events. Nature 370, 275–276 (1994). [27] Erkal, D. et al. The total mass of the Large Magellanic Cloud from its perturbation on the Orphan stream. MNRAS 487, 2685–2700 (2019). [28] Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. A&A 678, A208 (2023). [29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. A distance to the Large Magellanic Cloud that is precise to one per cent. Nature 567, 200–203 (2019). [42] Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. An H I Aperture Synthesis Mosaic of the Large Magellanic Cloud. ApJ 503, 674–688 (1998). [44] Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. The dark matter profile of the Milky Way inferred from its circular velocity curve. MNRAS 528, 693–710 (2024). [45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021). Jedamzik, K. Consistency of Primordial Black Hole Dark Matter with LIGO/Virgo Merger Rates. Phys. Rev. Lett. 126, 051302 (2021). [12] Escrivà, A., Bagui, E. & Clesse, S. Simulations of PBH formation at the QCD epoch and comparison with the GWTC-3 catalog. J. Cosmology Astropart. Phys 2023, 004 (2023). [13] Udalski, A., Szymański, M. K. & Szymański, G. OGLE-IV: Fourth Phase of the Optical Gravitational Lensing Experiment. Acta Astron. 65, 1–38 (2015). [14] Paczyński, B. Gravitational microlensing by the galactic halo. ApJ 304, 1–5 (1986). [15] Alcock, C. et al. The MACHO Project: Microlensing Results from 5.7 Years of Large Magellanic Cloud Observations. ApJ 542, 281–307 (2000). [16] Tisserand, P. et al. Limits on the Macho content of the Galactic Halo from the EROS-2 Survey of the Magellanic Clouds. A&A 469, 387–404 (2007). [17] Wyrzykowski, L. et al. The OGLE view of microlensing towards the Magellanic Clouds - IV. OGLE-III SMC data and final conclusions on MACHOs. MNRAS 416, 2949–2961 (2011). [18] Blaineau, T. et al. New limits from microlensing on Galactic black holes in the mass range 10 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT < M < 1000 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT. A&A 664, A106 (2022). [19] Udalski, A. The Optical Gravitational Lensing Experiment. Real Time Data Analysis Systems in the OGLE-III Survey. Acta Astron. 53, 291–305 (2003). [20] Mróz, P. et al. Microlensing optical depth and event rate toward the Large Magellanic Cloud based on 20 years of OGLE observations. submitted (2024). [21] Holtzman, J. A., Afonso, C. & Dolphin, A. The Local Group Stellar Populations Archive from the Hubble Space Telescope WFPC2. ApJS 166, 534–548 (2006). [22] Mróz, P. et al. No large population of unbound or wide-orbit Jupiter-mass planets. Nature 548, 183–186 (2017). [23] Cautun, M. et al. The milky way total mass profile as inferred from Gaia DR2. MNRAS 494, 4291–4313 (2020). [24] Han, C. & Gould, A. Stellar Contribution to the Galactic Bulge Microlensing Optical Depth. ApJ 592, 172–175 (2003). [25] Niikura, H. et al. Microlensing constraints on primordial black holes with Subaru/HSC Andromeda observations. Nature Astronomy 3, 524–534 (2019). [26] Sahu, K. C. Stars within the Large Magellanic Cloud as potential lenses for observed microlensing events. Nature 370, 275–276 (1994). [27] Erkal, D. et al. The total mass of the Large Magellanic Cloud from its perturbation on the Orphan stream. MNRAS 487, 2685–2700 (2019). [28] Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. A&A 678, A208 (2023). [29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. A distance to the Large Magellanic Cloud that is precise to one per cent. Nature 567, 200–203 (2019). [42] Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. An H I Aperture Synthesis Mosaic of the Large Magellanic Cloud. ApJ 503, 674–688 (1998). [44] Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. The dark matter profile of the Milky Way inferred from its circular velocity curve. MNRAS 528, 693–710 (2024). [45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021). Escrivà, A., Bagui, E. & Clesse, S. Simulations of PBH formation at the QCD epoch and comparison with the GWTC-3 catalog. J. Cosmology Astropart. Phys 2023, 004 (2023). [13] Udalski, A., Szymański, M. K. & Szymański, G. OGLE-IV: Fourth Phase of the Optical Gravitational Lensing Experiment. Acta Astron. 65, 1–38 (2015). [14] Paczyński, B. Gravitational microlensing by the galactic halo. ApJ 304, 1–5 (1986). [15] Alcock, C. et al. The MACHO Project: Microlensing Results from 5.7 Years of Large Magellanic Cloud Observations. ApJ 542, 281–307 (2000). [16] Tisserand, P. et al. Limits on the Macho content of the Galactic Halo from the EROS-2 Survey of the Magellanic Clouds. A&A 469, 387–404 (2007). [17] Wyrzykowski, L. et al. The OGLE view of microlensing towards the Magellanic Clouds - IV. OGLE-III SMC data and final conclusions on MACHOs. MNRAS 416, 2949–2961 (2011). [18] Blaineau, T. et al. New limits from microlensing on Galactic black holes in the mass range 10 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT < M < 1000 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT. A&A 664, A106 (2022). [19] Udalski, A. The Optical Gravitational Lensing Experiment. Real Time Data Analysis Systems in the OGLE-III Survey. Acta Astron. 53, 291–305 (2003). [20] Mróz, P. et al. Microlensing optical depth and event rate toward the Large Magellanic Cloud based on 20 years of OGLE observations. submitted (2024). [21] Holtzman, J. A., Afonso, C. & Dolphin, A. The Local Group Stellar Populations Archive from the Hubble Space Telescope WFPC2. ApJS 166, 534–548 (2006). [22] Mróz, P. et al. No large population of unbound or wide-orbit Jupiter-mass planets. Nature 548, 183–186 (2017). [23] Cautun, M. et al. The milky way total mass profile as inferred from Gaia DR2. MNRAS 494, 4291–4313 (2020). [24] Han, C. & Gould, A. Stellar Contribution to the Galactic Bulge Microlensing Optical Depth. ApJ 592, 172–175 (2003). [25] Niikura, H. et al. Microlensing constraints on primordial black holes with Subaru/HSC Andromeda observations. Nature Astronomy 3, 524–534 (2019). [26] Sahu, K. C. Stars within the Large Magellanic Cloud as potential lenses for observed microlensing events. Nature 370, 275–276 (1994). [27] Erkal, D. et al. The total mass of the Large Magellanic Cloud from its perturbation on the Orphan stream. MNRAS 487, 2685–2700 (2019). [28] Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. A&A 678, A208 (2023). [29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. A distance to the Large Magellanic Cloud that is precise to one per cent. Nature 567, 200–203 (2019). [42] Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. An H I Aperture Synthesis Mosaic of the Large Magellanic Cloud. ApJ 503, 674–688 (1998). [44] Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. The dark matter profile of the Milky Way inferred from its circular velocity curve. MNRAS 528, 693–710 (2024). [45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021). Udalski, A., Szymański, M. K. & Szymański, G. OGLE-IV: Fourth Phase of the Optical Gravitational Lensing Experiment. Acta Astron. 65, 1–38 (2015). [14] Paczyński, B. Gravitational microlensing by the galactic halo. ApJ 304, 1–5 (1986). [15] Alcock, C. et al. The MACHO Project: Microlensing Results from 5.7 Years of Large Magellanic Cloud Observations. ApJ 542, 281–307 (2000). [16] Tisserand, P. et al. Limits on the Macho content of the Galactic Halo from the EROS-2 Survey of the Magellanic Clouds. A&A 469, 387–404 (2007). [17] Wyrzykowski, L. et al. The OGLE view of microlensing towards the Magellanic Clouds - IV. OGLE-III SMC data and final conclusions on MACHOs. MNRAS 416, 2949–2961 (2011). [18] Blaineau, T. et al. New limits from microlensing on Galactic black holes in the mass range 10 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT < M < 1000 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT. A&A 664, A106 (2022). [19] Udalski, A. The Optical Gravitational Lensing Experiment. Real Time Data Analysis Systems in the OGLE-III Survey. Acta Astron. 53, 291–305 (2003). [20] Mróz, P. et al. Microlensing optical depth and event rate toward the Large Magellanic Cloud based on 20 years of OGLE observations. submitted (2024). [21] Holtzman, J. A., Afonso, C. & Dolphin, A. The Local Group Stellar Populations Archive from the Hubble Space Telescope WFPC2. ApJS 166, 534–548 (2006). [22] Mróz, P. et al. No large population of unbound or wide-orbit Jupiter-mass planets. Nature 548, 183–186 (2017). [23] Cautun, M. et al. The milky way total mass profile as inferred from Gaia DR2. MNRAS 494, 4291–4313 (2020). [24] Han, C. & Gould, A. Stellar Contribution to the Galactic Bulge Microlensing Optical Depth. ApJ 592, 172–175 (2003). [25] Niikura, H. et al. Microlensing constraints on primordial black holes with Subaru/HSC Andromeda observations. Nature Astronomy 3, 524–534 (2019). [26] Sahu, K. C. Stars within the Large Magellanic Cloud as potential lenses for observed microlensing events. Nature 370, 275–276 (1994). [27] Erkal, D. et al. The total mass of the Large Magellanic Cloud from its perturbation on the Orphan stream. MNRAS 487, 2685–2700 (2019). [28] Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. A&A 678, A208 (2023). [29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. A distance to the Large Magellanic Cloud that is precise to one per cent. Nature 567, 200–203 (2019). [42] Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. An H I Aperture Synthesis Mosaic of the Large Magellanic Cloud. ApJ 503, 674–688 (1998). [44] Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. The dark matter profile of the Milky Way inferred from its circular velocity curve. MNRAS 528, 693–710 (2024). [45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021). Paczyński, B. Gravitational microlensing by the galactic halo. ApJ 304, 1–5 (1986). [15] Alcock, C. et al. The MACHO Project: Microlensing Results from 5.7 Years of Large Magellanic Cloud Observations. ApJ 542, 281–307 (2000). [16] Tisserand, P. et al. Limits on the Macho content of the Galactic Halo from the EROS-2 Survey of the Magellanic Clouds. A&A 469, 387–404 (2007). [17] Wyrzykowski, L. et al. The OGLE view of microlensing towards the Magellanic Clouds - IV. OGLE-III SMC data and final conclusions on MACHOs. MNRAS 416, 2949–2961 (2011). [18] Blaineau, T. et al. New limits from microlensing on Galactic black holes in the mass range 10 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT < M < 1000 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT. A&A 664, A106 (2022). [19] Udalski, A. The Optical Gravitational Lensing Experiment. Real Time Data Analysis Systems in the OGLE-III Survey. Acta Astron. 53, 291–305 (2003). [20] Mróz, P. et al. Microlensing optical depth and event rate toward the Large Magellanic Cloud based on 20 years of OGLE observations. submitted (2024). [21] Holtzman, J. A., Afonso, C. & Dolphin, A. The Local Group Stellar Populations Archive from the Hubble Space Telescope WFPC2. ApJS 166, 534–548 (2006). [22] Mróz, P. et al. No large population of unbound or wide-orbit Jupiter-mass planets. Nature 548, 183–186 (2017). [23] Cautun, M. et al. The milky way total mass profile as inferred from Gaia DR2. MNRAS 494, 4291–4313 (2020). [24] Han, C. & Gould, A. Stellar Contribution to the Galactic Bulge Microlensing Optical Depth. ApJ 592, 172–175 (2003). [25] Niikura, H. et al. Microlensing constraints on primordial black holes with Subaru/HSC Andromeda observations. Nature Astronomy 3, 524–534 (2019). [26] Sahu, K. C. Stars within the Large Magellanic Cloud as potential lenses for observed microlensing events. Nature 370, 275–276 (1994). [27] Erkal, D. et al. The total mass of the Large Magellanic Cloud from its perturbation on the Orphan stream. MNRAS 487, 2685–2700 (2019). [28] Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. A&A 678, A208 (2023). [29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. A distance to the Large Magellanic Cloud that is precise to one per cent. Nature 567, 200–203 (2019). [42] Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. An H I Aperture Synthesis Mosaic of the Large Magellanic Cloud. ApJ 503, 674–688 (1998). [44] Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. The dark matter profile of the Milky Way inferred from its circular velocity curve. MNRAS 528, 693–710 (2024). [45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021). Alcock, C. et al. The MACHO Project: Microlensing Results from 5.7 Years of Large Magellanic Cloud Observations. ApJ 542, 281–307 (2000). [16] Tisserand, P. et al. Limits on the Macho content of the Galactic Halo from the EROS-2 Survey of the Magellanic Clouds. A&A 469, 387–404 (2007). [17] Wyrzykowski, L. et al. The OGLE view of microlensing towards the Magellanic Clouds - IV. OGLE-III SMC data and final conclusions on MACHOs. MNRAS 416, 2949–2961 (2011). [18] Blaineau, T. et al. New limits from microlensing on Galactic black holes in the mass range 10 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT < M < 1000 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT. A&A 664, A106 (2022). [19] Udalski, A. The Optical Gravitational Lensing Experiment. Real Time Data Analysis Systems in the OGLE-III Survey. Acta Astron. 53, 291–305 (2003). [20] Mróz, P. et al. Microlensing optical depth and event rate toward the Large Magellanic Cloud based on 20 years of OGLE observations. submitted (2024). [21] Holtzman, J. A., Afonso, C. & Dolphin, A. The Local Group Stellar Populations Archive from the Hubble Space Telescope WFPC2. ApJS 166, 534–548 (2006). [22] Mróz, P. et al. No large population of unbound or wide-orbit Jupiter-mass planets. Nature 548, 183–186 (2017). [23] Cautun, M. et al. The milky way total mass profile as inferred from Gaia DR2. MNRAS 494, 4291–4313 (2020). [24] Han, C. & Gould, A. Stellar Contribution to the Galactic Bulge Microlensing Optical Depth. ApJ 592, 172–175 (2003). [25] Niikura, H. et al. Microlensing constraints on primordial black holes with Subaru/HSC Andromeda observations. Nature Astronomy 3, 524–534 (2019). [26] Sahu, K. C. Stars within the Large Magellanic Cloud as potential lenses for observed microlensing events. Nature 370, 275–276 (1994). [27] Erkal, D. et al. The total mass of the Large Magellanic Cloud from its perturbation on the Orphan stream. MNRAS 487, 2685–2700 (2019). [28] Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. A&A 678, A208 (2023). [29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. A distance to the Large Magellanic Cloud that is precise to one per cent. Nature 567, 200–203 (2019). [42] Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. An H I Aperture Synthesis Mosaic of the Large Magellanic Cloud. ApJ 503, 674–688 (1998). [44] Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. The dark matter profile of the Milky Way inferred from its circular velocity curve. MNRAS 528, 693–710 (2024). [45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021). Tisserand, P. et al. Limits on the Macho content of the Galactic Halo from the EROS-2 Survey of the Magellanic Clouds. A&A 469, 387–404 (2007). [17] Wyrzykowski, L. et al. The OGLE view of microlensing towards the Magellanic Clouds - IV. OGLE-III SMC data and final conclusions on MACHOs. MNRAS 416, 2949–2961 (2011). [18] Blaineau, T. et al. New limits from microlensing on Galactic black holes in the mass range 10 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT < M < 1000 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT. A&A 664, A106 (2022). [19] Udalski, A. The Optical Gravitational Lensing Experiment. Real Time Data Analysis Systems in the OGLE-III Survey. Acta Astron. 53, 291–305 (2003). [20] Mróz, P. et al. Microlensing optical depth and event rate toward the Large Magellanic Cloud based on 20 years of OGLE observations. submitted (2024). [21] Holtzman, J. A., Afonso, C. & Dolphin, A. The Local Group Stellar Populations Archive from the Hubble Space Telescope WFPC2. ApJS 166, 534–548 (2006). [22] Mróz, P. et al. No large population of unbound or wide-orbit Jupiter-mass planets. Nature 548, 183–186 (2017). [23] Cautun, M. et al. The milky way total mass profile as inferred from Gaia DR2. MNRAS 494, 4291–4313 (2020). [24] Han, C. & Gould, A. Stellar Contribution to the Galactic Bulge Microlensing Optical Depth. ApJ 592, 172–175 (2003). [25] Niikura, H. et al. Microlensing constraints on primordial black holes with Subaru/HSC Andromeda observations. Nature Astronomy 3, 524–534 (2019). [26] Sahu, K. C. Stars within the Large Magellanic Cloud as potential lenses for observed microlensing events. Nature 370, 275–276 (1994). [27] Erkal, D. et al. The total mass of the Large Magellanic Cloud from its perturbation on the Orphan stream. MNRAS 487, 2685–2700 (2019). [28] Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. A&A 678, A208 (2023). [29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. 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The Local Group Stellar Populations Archive from the Hubble Space Telescope WFPC2. ApJS 166, 534–548 (2006). [22] Mróz, P. et al. No large population of unbound or wide-orbit Jupiter-mass planets. Nature 548, 183–186 (2017). [23] Cautun, M. et al. The milky way total mass profile as inferred from Gaia DR2. MNRAS 494, 4291–4313 (2020). [24] Han, C. & Gould, A. Stellar Contribution to the Galactic Bulge Microlensing Optical Depth. ApJ 592, 172–175 (2003). [25] Niikura, H. et al. Microlensing constraints on primordial black holes with Subaru/HSC Andromeda observations. Nature Astronomy 3, 524–534 (2019). [26] Sahu, K. C. Stars within the Large Magellanic Cloud as potential lenses for observed microlensing events. Nature 370, 275–276 (1994). [27] Erkal, D. et al. The total mass of the Large Magellanic Cloud from its perturbation on the Orphan stream. MNRAS 487, 2685–2700 (2019). [28] Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. A&A 678, A208 (2023). [29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. A distance to the Large Magellanic Cloud that is precise to one per cent. Nature 567, 200–203 (2019). [42] Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. An H I Aperture Synthesis Mosaic of the Large Magellanic Cloud. ApJ 503, 674–688 (1998). [44] Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. The dark matter profile of the Milky Way inferred from its circular velocity curve. MNRAS 528, 693–710 (2024). [45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021). Blaineau, T. et al. New limits from microlensing on Galactic black holes in the mass range 10 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT < M < 1000 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT. A&A 664, A106 (2022). [19] Udalski, A. The Optical Gravitational Lensing Experiment. Real Time Data Analysis Systems in the OGLE-III Survey. Acta Astron. 53, 291–305 (2003). [20] Mróz, P. et al. Microlensing optical depth and event rate toward the Large Magellanic Cloud based on 20 years of OGLE observations. submitted (2024). [21] Holtzman, J. A., Afonso, C. & Dolphin, A. The Local Group Stellar Populations Archive from the Hubble Space Telescope WFPC2. ApJS 166, 534–548 (2006). [22] Mróz, P. et al. No large population of unbound or wide-orbit Jupiter-mass planets. Nature 548, 183–186 (2017). [23] Cautun, M. et al. The milky way total mass profile as inferred from Gaia DR2. MNRAS 494, 4291–4313 (2020). [24] Han, C. & Gould, A. Stellar Contribution to the Galactic Bulge Microlensing Optical Depth. ApJ 592, 172–175 (2003). [25] Niikura, H. et al. Microlensing constraints on primordial black holes with Subaru/HSC Andromeda observations. Nature Astronomy 3, 524–534 (2019). [26] Sahu, K. C. Stars within the Large Magellanic Cloud as potential lenses for observed microlensing events. Nature 370, 275–276 (1994). [27] Erkal, D. et al. The total mass of the Large Magellanic Cloud from its perturbation on the Orphan stream. MNRAS 487, 2685–2700 (2019). [28] Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. A&A 678, A208 (2023). [29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. A distance to the Large Magellanic Cloud that is precise to one per cent. Nature 567, 200–203 (2019). [42] Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. An H I Aperture Synthesis Mosaic of the Large Magellanic Cloud. ApJ 503, 674–688 (1998). [44] Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. The dark matter profile of the Milky Way inferred from its circular velocity curve. MNRAS 528, 693–710 (2024). [45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021). Udalski, A. The Optical Gravitational Lensing Experiment. Real Time Data Analysis Systems in the OGLE-III Survey. Acta Astron. 53, 291–305 (2003). [20] Mróz, P. et al. Microlensing optical depth and event rate toward the Large Magellanic Cloud based on 20 years of OGLE observations. submitted (2024). [21] Holtzman, J. A., Afonso, C. & Dolphin, A. The Local Group Stellar Populations Archive from the Hubble Space Telescope WFPC2. ApJS 166, 534–548 (2006). [22] Mróz, P. et al. No large population of unbound or wide-orbit Jupiter-mass planets. Nature 548, 183–186 (2017). [23] Cautun, M. et al. The milky way total mass profile as inferred from Gaia DR2. MNRAS 494, 4291–4313 (2020). [24] Han, C. & Gould, A. Stellar Contribution to the Galactic Bulge Microlensing Optical Depth. ApJ 592, 172–175 (2003). [25] Niikura, H. et al. Microlensing constraints on primordial black holes with Subaru/HSC Andromeda observations. Nature Astronomy 3, 524–534 (2019). [26] Sahu, K. C. Stars within the Large Magellanic Cloud as potential lenses for observed microlensing events. Nature 370, 275–276 (1994). [27] Erkal, D. et al. The total mass of the Large Magellanic Cloud from its perturbation on the Orphan stream. MNRAS 487, 2685–2700 (2019). [28] Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. A&A 678, A208 (2023). [29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. A distance to the Large Magellanic Cloud that is precise to one per cent. Nature 567, 200–203 (2019). [42] Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. An H I Aperture Synthesis Mosaic of the Large Magellanic Cloud. ApJ 503, 674–688 (1998). [44] Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. The dark matter profile of the Milky Way inferred from its circular velocity curve. MNRAS 528, 693–710 (2024). [45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021). Mróz, P. et al. Microlensing optical depth and event rate toward the Large Magellanic Cloud based on 20 years of OGLE observations. submitted (2024). [21] Holtzman, J. A., Afonso, C. & Dolphin, A. The Local Group Stellar Populations Archive from the Hubble Space Telescope WFPC2. ApJS 166, 534–548 (2006). [22] Mróz, P. et al. No large population of unbound or wide-orbit Jupiter-mass planets. Nature 548, 183–186 (2017). [23] Cautun, M. et al. The milky way total mass profile as inferred from Gaia DR2. MNRAS 494, 4291–4313 (2020). [24] Han, C. & Gould, A. Stellar Contribution to the Galactic Bulge Microlensing Optical Depth. ApJ 592, 172–175 (2003). [25] Niikura, H. et al. Microlensing constraints on primordial black holes with Subaru/HSC Andromeda observations. Nature Astronomy 3, 524–534 (2019). [26] Sahu, K. C. Stars within the Large Magellanic Cloud as potential lenses for observed microlensing events. Nature 370, 275–276 (1994). [27] Erkal, D. et al. The total mass of the Large Magellanic Cloud from its perturbation on the Orphan stream. MNRAS 487, 2685–2700 (2019). [28] Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. A&A 678, A208 (2023). [29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. A distance to the Large Magellanic Cloud that is precise to one per cent. Nature 567, 200–203 (2019). [42] Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. An H I Aperture Synthesis Mosaic of the Large Magellanic Cloud. ApJ 503, 674–688 (1998). [44] Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. The dark matter profile of the Milky Way inferred from its circular velocity curve. MNRAS 528, 693–710 (2024). [45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021). Holtzman, J. A., Afonso, C. & Dolphin, A. The Local Group Stellar Populations Archive from the Hubble Space Telescope WFPC2. ApJS 166, 534–548 (2006). [22] Mróz, P. et al. No large population of unbound or wide-orbit Jupiter-mass planets. Nature 548, 183–186 (2017). [23] Cautun, M. et al. The milky way total mass profile as inferred from Gaia DR2. MNRAS 494, 4291–4313 (2020). [24] Han, C. & Gould, A. Stellar Contribution to the Galactic Bulge Microlensing Optical Depth. ApJ 592, 172–175 (2003). [25] Niikura, H. et al. Microlensing constraints on primordial black holes with Subaru/HSC Andromeda observations. Nature Astronomy 3, 524–534 (2019). [26] Sahu, K. C. Stars within the Large Magellanic Cloud as potential lenses for observed microlensing events. Nature 370, 275–276 (1994). [27] Erkal, D. et al. The total mass of the Large Magellanic Cloud from its perturbation on the Orphan stream. MNRAS 487, 2685–2700 (2019). [28] Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. A&A 678, A208 (2023). [29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. 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Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. A distance to the Large Magellanic Cloud that is precise to one per cent. Nature 567, 200–203 (2019). [42] Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. An H I Aperture Synthesis Mosaic of the Large Magellanic Cloud. ApJ 503, 674–688 (1998). [44] Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. The dark matter profile of the Milky Way inferred from its circular velocity curve. MNRAS 528, 693–710 (2024). [45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021). Clesse, S. & García-Bellido, J. The clustering of massive Primordial Black Holes as Dark Matter: Measuring their mass distribution with advanced LIGO. Phys. Dark Universe 15, 142–147 (2017). [10] Carr, B., Clesse, S., García-Bellido, J. & Kühnel, F. Cosmic conundra explained by thermal history and primordial black holes. Phys. Dark Universe 31, 100755 (2021). [11] Jedamzik, K. Consistency of Primordial Black Hole Dark Matter with LIGO/Virgo Merger Rates. Phys. Rev. Lett. 126, 051302 (2021). [12] Escrivà, A., Bagui, E. & Clesse, S. Simulations of PBH formation at the QCD epoch and comparison with the GWTC-3 catalog. J. Cosmology Astropart. Phys 2023, 004 (2023). [13] Udalski, A., Szymański, M. K. & Szymański, G. OGLE-IV: Fourth Phase of the Optical Gravitational Lensing Experiment. Acta Astron. 65, 1–38 (2015). [14] Paczyński, B. Gravitational microlensing by the galactic halo. ApJ 304, 1–5 (1986). [15] Alcock, C. et al. The MACHO Project: Microlensing Results from 5.7 Years of Large Magellanic Cloud Observations. ApJ 542, 281–307 (2000). [16] Tisserand, P. et al. Limits on the Macho content of the Galactic Halo from the EROS-2 Survey of the Magellanic Clouds. A&A 469, 387–404 (2007). [17] Wyrzykowski, L. et al. The OGLE view of microlensing towards the Magellanic Clouds - IV. OGLE-III SMC data and final conclusions on MACHOs. MNRAS 416, 2949–2961 (2011). [18] Blaineau, T. et al. New limits from microlensing on Galactic black holes in the mass range 10 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT < M < 1000 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT. A&A 664, A106 (2022). [19] Udalski, A. The Optical Gravitational Lensing Experiment. Real Time Data Analysis Systems in the OGLE-III Survey. Acta Astron. 53, 291–305 (2003). [20] Mróz, P. et al. Microlensing optical depth and event rate toward the Large Magellanic Cloud based on 20 years of OGLE observations. submitted (2024). [21] Holtzman, J. A., Afonso, C. & Dolphin, A. The Local Group Stellar Populations Archive from the Hubble Space Telescope WFPC2. ApJS 166, 534–548 (2006). [22] Mróz, P. et al. No large population of unbound or wide-orbit Jupiter-mass planets. Nature 548, 183–186 (2017). [23] Cautun, M. et al. The milky way total mass profile as inferred from Gaia DR2. MNRAS 494, 4291–4313 (2020). [24] Han, C. & Gould, A. Stellar Contribution to the Galactic Bulge Microlensing Optical Depth. ApJ 592, 172–175 (2003). [25] Niikura, H. et al. Microlensing constraints on primordial black holes with Subaru/HSC Andromeda observations. Nature Astronomy 3, 524–534 (2019). [26] Sahu, K. C. Stars within the Large Magellanic Cloud as potential lenses for observed microlensing events. Nature 370, 275–276 (1994). [27] Erkal, D. et al. The total mass of the Large Magellanic Cloud from its perturbation on the Orphan stream. MNRAS 487, 2685–2700 (2019). [28] Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. A&A 678, A208 (2023). [29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. A distance to the Large Magellanic Cloud that is precise to one per cent. Nature 567, 200–203 (2019). [42] Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. An H I Aperture Synthesis Mosaic of the Large Magellanic Cloud. ApJ 503, 674–688 (1998). [44] Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. The dark matter profile of the Milky Way inferred from its circular velocity curve. MNRAS 528, 693–710 (2024). [45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021). Carr, B., Clesse, S., García-Bellido, J. & Kühnel, F. Cosmic conundra explained by thermal history and primordial black holes. Phys. Dark Universe 31, 100755 (2021). [11] Jedamzik, K. Consistency of Primordial Black Hole Dark Matter with LIGO/Virgo Merger Rates. Phys. Rev. Lett. 126, 051302 (2021). [12] Escrivà, A., Bagui, E. & Clesse, S. Simulations of PBH formation at the QCD epoch and comparison with the GWTC-3 catalog. J. Cosmology Astropart. Phys 2023, 004 (2023). [13] Udalski, A., Szymański, M. K. & Szymański, G. OGLE-IV: Fourth Phase of the Optical Gravitational Lensing Experiment. Acta Astron. 65, 1–38 (2015). [14] Paczyński, B. Gravitational microlensing by the galactic halo. ApJ 304, 1–5 (1986). [15] Alcock, C. et al. The MACHO Project: Microlensing Results from 5.7 Years of Large Magellanic Cloud Observations. ApJ 542, 281–307 (2000). [16] Tisserand, P. et al. Limits on the Macho content of the Galactic Halo from the EROS-2 Survey of the Magellanic Clouds. A&A 469, 387–404 (2007). [17] Wyrzykowski, L. et al. The OGLE view of microlensing towards the Magellanic Clouds - IV. OGLE-III SMC data and final conclusions on MACHOs. MNRAS 416, 2949–2961 (2011). [18] Blaineau, T. et al. New limits from microlensing on Galactic black holes in the mass range 10 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT < M < 1000 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT. A&A 664, A106 (2022). [19] Udalski, A. The Optical Gravitational Lensing Experiment. Real Time Data Analysis Systems in the OGLE-III Survey. Acta Astron. 53, 291–305 (2003). [20] Mróz, P. et al. Microlensing optical depth and event rate toward the Large Magellanic Cloud based on 20 years of OGLE observations. submitted (2024). [21] Holtzman, J. A., Afonso, C. & Dolphin, A. The Local Group Stellar Populations Archive from the Hubble Space Telescope WFPC2. ApJS 166, 534–548 (2006). [22] Mróz, P. et al. No large population of unbound or wide-orbit Jupiter-mass planets. Nature 548, 183–186 (2017). [23] Cautun, M. et al. The milky way total mass profile as inferred from Gaia DR2. MNRAS 494, 4291–4313 (2020). [24] Han, C. & Gould, A. Stellar Contribution to the Galactic Bulge Microlensing Optical Depth. ApJ 592, 172–175 (2003). [25] Niikura, H. et al. Microlensing constraints on primordial black holes with Subaru/HSC Andromeda observations. Nature Astronomy 3, 524–534 (2019). [26] Sahu, K. C. Stars within the Large Magellanic Cloud as potential lenses for observed microlensing events. Nature 370, 275–276 (1994). [27] Erkal, D. et al. The total mass of the Large Magellanic Cloud from its perturbation on the Orphan stream. MNRAS 487, 2685–2700 (2019). [28] Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. A&A 678, A208 (2023). [29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. A distance to the Large Magellanic Cloud that is precise to one per cent. Nature 567, 200–203 (2019). [42] Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. An H I Aperture Synthesis Mosaic of the Large Magellanic Cloud. ApJ 503, 674–688 (1998). [44] Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. The dark matter profile of the Milky Way inferred from its circular velocity curve. MNRAS 528, 693–710 (2024). [45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021). Jedamzik, K. Consistency of Primordial Black Hole Dark Matter with LIGO/Virgo Merger Rates. Phys. Rev. Lett. 126, 051302 (2021). [12] Escrivà, A., Bagui, E. & Clesse, S. Simulations of PBH formation at the QCD epoch and comparison with the GWTC-3 catalog. J. Cosmology Astropart. Phys 2023, 004 (2023). [13] Udalski, A., Szymański, M. K. & Szymański, G. OGLE-IV: Fourth Phase of the Optical Gravitational Lensing Experiment. Acta Astron. 65, 1–38 (2015). [14] Paczyński, B. Gravitational microlensing by the galactic halo. ApJ 304, 1–5 (1986). [15] Alcock, C. et al. The MACHO Project: Microlensing Results from 5.7 Years of Large Magellanic Cloud Observations. ApJ 542, 281–307 (2000). [16] Tisserand, P. et al. Limits on the Macho content of the Galactic Halo from the EROS-2 Survey of the Magellanic Clouds. A&A 469, 387–404 (2007). [17] Wyrzykowski, L. et al. The OGLE view of microlensing towards the Magellanic Clouds - IV. OGLE-III SMC data and final conclusions on MACHOs. MNRAS 416, 2949–2961 (2011). [18] Blaineau, T. et al. New limits from microlensing on Galactic black holes in the mass range 10 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT < M < 1000 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT. A&A 664, A106 (2022). [19] Udalski, A. The Optical Gravitational Lensing Experiment. Real Time Data Analysis Systems in the OGLE-III Survey. Acta Astron. 53, 291–305 (2003). [20] Mróz, P. et al. Microlensing optical depth and event rate toward the Large Magellanic Cloud based on 20 years of OGLE observations. submitted (2024). [21] Holtzman, J. A., Afonso, C. & Dolphin, A. The Local Group Stellar Populations Archive from the Hubble Space Telescope WFPC2. ApJS 166, 534–548 (2006). [22] Mróz, P. et al. No large population of unbound or wide-orbit Jupiter-mass planets. Nature 548, 183–186 (2017). [23] Cautun, M. et al. The milky way total mass profile as inferred from Gaia DR2. MNRAS 494, 4291–4313 (2020). [24] Han, C. & Gould, A. Stellar Contribution to the Galactic Bulge Microlensing Optical Depth. ApJ 592, 172–175 (2003). [25] Niikura, H. et al. Microlensing constraints on primordial black holes with Subaru/HSC Andromeda observations. Nature Astronomy 3, 524–534 (2019). [26] Sahu, K. C. Stars within the Large Magellanic Cloud as potential lenses for observed microlensing events. Nature 370, 275–276 (1994). [27] Erkal, D. et al. The total mass of the Large Magellanic Cloud from its perturbation on the Orphan stream. MNRAS 487, 2685–2700 (2019). [28] Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. A&A 678, A208 (2023). [29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. A distance to the Large Magellanic Cloud that is precise to one per cent. Nature 567, 200–203 (2019). [42] Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. An H I Aperture Synthesis Mosaic of the Large Magellanic Cloud. ApJ 503, 674–688 (1998). [44] Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. The dark matter profile of the Milky Way inferred from its circular velocity curve. MNRAS 528, 693–710 (2024). [45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021). Escrivà, A., Bagui, E. & Clesse, S. Simulations of PBH formation at the QCD epoch and comparison with the GWTC-3 catalog. J. Cosmology Astropart. Phys 2023, 004 (2023). [13] Udalski, A., Szymański, M. K. & Szymański, G. OGLE-IV: Fourth Phase of the Optical Gravitational Lensing Experiment. Acta Astron. 65, 1–38 (2015). [14] Paczyński, B. Gravitational microlensing by the galactic halo. ApJ 304, 1–5 (1986). [15] Alcock, C. et al. The MACHO Project: Microlensing Results from 5.7 Years of Large Magellanic Cloud Observations. ApJ 542, 281–307 (2000). [16] Tisserand, P. et al. Limits on the Macho content of the Galactic Halo from the EROS-2 Survey of the Magellanic Clouds. A&A 469, 387–404 (2007). [17] Wyrzykowski, L. et al. The OGLE view of microlensing towards the Magellanic Clouds - IV. OGLE-III SMC data and final conclusions on MACHOs. MNRAS 416, 2949–2961 (2011). [18] Blaineau, T. et al. New limits from microlensing on Galactic black holes in the mass range 10 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT < M < 1000 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT. A&A 664, A106 (2022). [19] Udalski, A. The Optical Gravitational Lensing Experiment. Real Time Data Analysis Systems in the OGLE-III Survey. Acta Astron. 53, 291–305 (2003). [20] Mróz, P. et al. Microlensing optical depth and event rate toward the Large Magellanic Cloud based on 20 years of OGLE observations. submitted (2024). [21] Holtzman, J. A., Afonso, C. & Dolphin, A. The Local Group Stellar Populations Archive from the Hubble Space Telescope WFPC2. ApJS 166, 534–548 (2006). [22] Mróz, P. et al. No large population of unbound or wide-orbit Jupiter-mass planets. Nature 548, 183–186 (2017). [23] Cautun, M. et al. The milky way total mass profile as inferred from Gaia DR2. MNRAS 494, 4291–4313 (2020). [24] Han, C. & Gould, A. Stellar Contribution to the Galactic Bulge Microlensing Optical Depth. ApJ 592, 172–175 (2003). [25] Niikura, H. et al. Microlensing constraints on primordial black holes with Subaru/HSC Andromeda observations. Nature Astronomy 3, 524–534 (2019). [26] Sahu, K. C. Stars within the Large Magellanic Cloud as potential lenses for observed microlensing events. Nature 370, 275–276 (1994). [27] Erkal, D. et al. The total mass of the Large Magellanic Cloud from its perturbation on the Orphan stream. MNRAS 487, 2685–2700 (2019). [28] Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. A&A 678, A208 (2023). [29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. A distance to the Large Magellanic Cloud that is precise to one per cent. Nature 567, 200–203 (2019). [42] Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. An H I Aperture Synthesis Mosaic of the Large Magellanic Cloud. ApJ 503, 674–688 (1998). [44] Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. The dark matter profile of the Milky Way inferred from its circular velocity curve. MNRAS 528, 693–710 (2024). [45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021). Udalski, A., Szymański, M. K. & Szymański, G. OGLE-IV: Fourth Phase of the Optical Gravitational Lensing Experiment. Acta Astron. 65, 1–38 (2015). [14] Paczyński, B. Gravitational microlensing by the galactic halo. ApJ 304, 1–5 (1986). [15] Alcock, C. et al. The MACHO Project: Microlensing Results from 5.7 Years of Large Magellanic Cloud Observations. ApJ 542, 281–307 (2000). [16] Tisserand, P. et al. Limits on the Macho content of the Galactic Halo from the EROS-2 Survey of the Magellanic Clouds. A&A 469, 387–404 (2007). [17] Wyrzykowski, L. et al. The OGLE view of microlensing towards the Magellanic Clouds - IV. OGLE-III SMC data and final conclusions on MACHOs. MNRAS 416, 2949–2961 (2011). [18] Blaineau, T. et al. New limits from microlensing on Galactic black holes in the mass range 10 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT < M < 1000 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT. A&A 664, A106 (2022). [19] Udalski, A. The Optical Gravitational Lensing Experiment. Real Time Data Analysis Systems in the OGLE-III Survey. Acta Astron. 53, 291–305 (2003). [20] Mróz, P. et al. Microlensing optical depth and event rate toward the Large Magellanic Cloud based on 20 years of OGLE observations. submitted (2024). [21] Holtzman, J. A., Afonso, C. & Dolphin, A. The Local Group Stellar Populations Archive from the Hubble Space Telescope WFPC2. ApJS 166, 534–548 (2006). [22] Mróz, P. et al. No large population of unbound or wide-orbit Jupiter-mass planets. Nature 548, 183–186 (2017). [23] Cautun, M. et al. The milky way total mass profile as inferred from Gaia DR2. MNRAS 494, 4291–4313 (2020). [24] Han, C. & Gould, A. Stellar Contribution to the Galactic Bulge Microlensing Optical Depth. ApJ 592, 172–175 (2003). [25] Niikura, H. et al. Microlensing constraints on primordial black holes with Subaru/HSC Andromeda observations. Nature Astronomy 3, 524–534 (2019). [26] Sahu, K. C. Stars within the Large Magellanic Cloud as potential lenses for observed microlensing events. Nature 370, 275–276 (1994). [27] Erkal, D. et al. The total mass of the Large Magellanic Cloud from its perturbation on the Orphan stream. MNRAS 487, 2685–2700 (2019). [28] Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. A&A 678, A208 (2023). [29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. A distance to the Large Magellanic Cloud that is precise to one per cent. Nature 567, 200–203 (2019). [42] Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. An H I Aperture Synthesis Mosaic of the Large Magellanic Cloud. ApJ 503, 674–688 (1998). [44] Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. The dark matter profile of the Milky Way inferred from its circular velocity curve. MNRAS 528, 693–710 (2024). [45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021). Paczyński, B. Gravitational microlensing by the galactic halo. ApJ 304, 1–5 (1986). [15] Alcock, C. et al. The MACHO Project: Microlensing Results from 5.7 Years of Large Magellanic Cloud Observations. ApJ 542, 281–307 (2000). [16] Tisserand, P. et al. Limits on the Macho content of the Galactic Halo from the EROS-2 Survey of the Magellanic Clouds. A&A 469, 387–404 (2007). [17] Wyrzykowski, L. et al. The OGLE view of microlensing towards the Magellanic Clouds - IV. OGLE-III SMC data and final conclusions on MACHOs. MNRAS 416, 2949–2961 (2011). [18] Blaineau, T. et al. New limits from microlensing on Galactic black holes in the mass range 10 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT < M < 1000 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT. A&A 664, A106 (2022). [19] Udalski, A. The Optical Gravitational Lensing Experiment. Real Time Data Analysis Systems in the OGLE-III Survey. Acta Astron. 53, 291–305 (2003). [20] Mróz, P. et al. Microlensing optical depth and event rate toward the Large Magellanic Cloud based on 20 years of OGLE observations. submitted (2024). [21] Holtzman, J. A., Afonso, C. & Dolphin, A. The Local Group Stellar Populations Archive from the Hubble Space Telescope WFPC2. ApJS 166, 534–548 (2006). [22] Mróz, P. et al. No large population of unbound or wide-orbit Jupiter-mass planets. Nature 548, 183–186 (2017). [23] Cautun, M. et al. The milky way total mass profile as inferred from Gaia DR2. MNRAS 494, 4291–4313 (2020). [24] Han, C. & Gould, A. Stellar Contribution to the Galactic Bulge Microlensing Optical Depth. ApJ 592, 172–175 (2003). [25] Niikura, H. et al. Microlensing constraints on primordial black holes with Subaru/HSC Andromeda observations. Nature Astronomy 3, 524–534 (2019). [26] Sahu, K. C. Stars within the Large Magellanic Cloud as potential lenses for observed microlensing events. Nature 370, 275–276 (1994). [27] Erkal, D. et al. The total mass of the Large Magellanic Cloud from its perturbation on the Orphan stream. MNRAS 487, 2685–2700 (2019). [28] Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. A&A 678, A208 (2023). [29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. A distance to the Large Magellanic Cloud that is precise to one per cent. Nature 567, 200–203 (2019). [42] Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. An H I Aperture Synthesis Mosaic of the Large Magellanic Cloud. ApJ 503, 674–688 (1998). [44] Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. The dark matter profile of the Milky Way inferred from its circular velocity curve. MNRAS 528, 693–710 (2024). [45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021). Alcock, C. et al. The MACHO Project: Microlensing Results from 5.7 Years of Large Magellanic Cloud Observations. ApJ 542, 281–307 (2000). [16] Tisserand, P. et al. Limits on the Macho content of the Galactic Halo from the EROS-2 Survey of the Magellanic Clouds. A&A 469, 387–404 (2007). [17] Wyrzykowski, L. et al. The OGLE view of microlensing towards the Magellanic Clouds - IV. OGLE-III SMC data and final conclusions on MACHOs. MNRAS 416, 2949–2961 (2011). [18] Blaineau, T. et al. New limits from microlensing on Galactic black holes in the mass range 10 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT < M < 1000 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT. A&A 664, A106 (2022). [19] Udalski, A. The Optical Gravitational Lensing Experiment. Real Time Data Analysis Systems in the OGLE-III Survey. Acta Astron. 53, 291–305 (2003). [20] Mróz, P. et al. Microlensing optical depth and event rate toward the Large Magellanic Cloud based on 20 years of OGLE observations. submitted (2024). [21] Holtzman, J. A., Afonso, C. & Dolphin, A. The Local Group Stellar Populations Archive from the Hubble Space Telescope WFPC2. ApJS 166, 534–548 (2006). [22] Mróz, P. et al. No large population of unbound or wide-orbit Jupiter-mass planets. Nature 548, 183–186 (2017). [23] Cautun, M. et al. The milky way total mass profile as inferred from Gaia DR2. MNRAS 494, 4291–4313 (2020). [24] Han, C. & Gould, A. Stellar Contribution to the Galactic Bulge Microlensing Optical Depth. ApJ 592, 172–175 (2003). [25] Niikura, H. et al. Microlensing constraints on primordial black holes with Subaru/HSC Andromeda observations. Nature Astronomy 3, 524–534 (2019). [26] Sahu, K. C. Stars within the Large Magellanic Cloud as potential lenses for observed microlensing events. Nature 370, 275–276 (1994). [27] Erkal, D. et al. The total mass of the Large Magellanic Cloud from its perturbation on the Orphan stream. MNRAS 487, 2685–2700 (2019). [28] Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. A&A 678, A208 (2023). [29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. A distance to the Large Magellanic Cloud that is precise to one per cent. Nature 567, 200–203 (2019). [42] Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. An H I Aperture Synthesis Mosaic of the Large Magellanic Cloud. ApJ 503, 674–688 (1998). [44] Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. The dark matter profile of the Milky Way inferred from its circular velocity curve. MNRAS 528, 693–710 (2024). [45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021). Tisserand, P. et al. Limits on the Macho content of the Galactic Halo from the EROS-2 Survey of the Magellanic Clouds. A&A 469, 387–404 (2007). [17] Wyrzykowski, L. et al. The OGLE view of microlensing towards the Magellanic Clouds - IV. OGLE-III SMC data and final conclusions on MACHOs. MNRAS 416, 2949–2961 (2011). [18] Blaineau, T. et al. New limits from microlensing on Galactic black holes in the mass range 10 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT < M < 1000 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT. A&A 664, A106 (2022). [19] Udalski, A. The Optical Gravitational Lensing Experiment. Real Time Data Analysis Systems in the OGLE-III Survey. Acta Astron. 53, 291–305 (2003). [20] Mróz, P. et al. Microlensing optical depth and event rate toward the Large Magellanic Cloud based on 20 years of OGLE observations. submitted (2024). [21] Holtzman, J. A., Afonso, C. & Dolphin, A. The Local Group Stellar Populations Archive from the Hubble Space Telescope WFPC2. ApJS 166, 534–548 (2006). [22] Mróz, P. et al. No large population of unbound or wide-orbit Jupiter-mass planets. Nature 548, 183–186 (2017). [23] Cautun, M. et al. The milky way total mass profile as inferred from Gaia DR2. MNRAS 494, 4291–4313 (2020). [24] Han, C. & Gould, A. Stellar Contribution to the Galactic Bulge Microlensing Optical Depth. ApJ 592, 172–175 (2003). [25] Niikura, H. et al. Microlensing constraints on primordial black holes with Subaru/HSC Andromeda observations. Nature Astronomy 3, 524–534 (2019). [26] Sahu, K. C. Stars within the Large Magellanic Cloud as potential lenses for observed microlensing events. Nature 370, 275–276 (1994). [27] Erkal, D. et al. The total mass of the Large Magellanic Cloud from its perturbation on the Orphan stream. MNRAS 487, 2685–2700 (2019). [28] Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. A&A 678, A208 (2023). [29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. A distance to the Large Magellanic Cloud that is precise to one per cent. Nature 567, 200–203 (2019). [42] Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. An H I Aperture Synthesis Mosaic of the Large Magellanic Cloud. ApJ 503, 674–688 (1998). [44] Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. The dark matter profile of the Milky Way inferred from its circular velocity curve. MNRAS 528, 693–710 (2024). [45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021). Wyrzykowski, L. et al. The OGLE view of microlensing towards the Magellanic Clouds - IV. OGLE-III SMC data and final conclusions on MACHOs. MNRAS 416, 2949–2961 (2011). [18] Blaineau, T. et al. New limits from microlensing on Galactic black holes in the mass range 10 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT < M < 1000 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT. A&A 664, A106 (2022). [19] Udalski, A. The Optical Gravitational Lensing Experiment. Real Time Data Analysis Systems in the OGLE-III Survey. Acta Astron. 53, 291–305 (2003). [20] Mróz, P. et al. Microlensing optical depth and event rate toward the Large Magellanic Cloud based on 20 years of OGLE observations. submitted (2024). [21] Holtzman, J. A., Afonso, C. & Dolphin, A. The Local Group Stellar Populations Archive from the Hubble Space Telescope WFPC2. ApJS 166, 534–548 (2006). [22] Mróz, P. et al. No large population of unbound or wide-orbit Jupiter-mass planets. Nature 548, 183–186 (2017). [23] Cautun, M. et al. The milky way total mass profile as inferred from Gaia DR2. MNRAS 494, 4291–4313 (2020). [24] Han, C. & Gould, A. Stellar Contribution to the Galactic Bulge Microlensing Optical Depth. ApJ 592, 172–175 (2003). [25] Niikura, H. et al. Microlensing constraints on primordial black holes with Subaru/HSC Andromeda observations. Nature Astronomy 3, 524–534 (2019). [26] Sahu, K. C. Stars within the Large Magellanic Cloud as potential lenses for observed microlensing events. Nature 370, 275–276 (1994). [27] Erkal, D. et al. The total mass of the Large Magellanic Cloud from its perturbation on the Orphan stream. MNRAS 487, 2685–2700 (2019). [28] Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. A&A 678, A208 (2023). [29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. A distance to the Large Magellanic Cloud that is precise to one per cent. Nature 567, 200–203 (2019). [42] Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. An H I Aperture Synthesis Mosaic of the Large Magellanic Cloud. ApJ 503, 674–688 (1998). [44] Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. The dark matter profile of the Milky Way inferred from its circular velocity curve. MNRAS 528, 693–710 (2024). [45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021). Blaineau, T. et al. New limits from microlensing on Galactic black holes in the mass range 10 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT < M < 1000 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT. A&A 664, A106 (2022). [19] Udalski, A. The Optical Gravitational Lensing Experiment. Real Time Data Analysis Systems in the OGLE-III Survey. Acta Astron. 53, 291–305 (2003). [20] Mróz, P. et al. Microlensing optical depth and event rate toward the Large Magellanic Cloud based on 20 years of OGLE observations. submitted (2024). [21] Holtzman, J. A., Afonso, C. & Dolphin, A. The Local Group Stellar Populations Archive from the Hubble Space Telescope WFPC2. ApJS 166, 534–548 (2006). [22] Mróz, P. et al. No large population of unbound or wide-orbit Jupiter-mass planets. Nature 548, 183–186 (2017). [23] Cautun, M. et al. The milky way total mass profile as inferred from Gaia DR2. MNRAS 494, 4291–4313 (2020). [24] Han, C. & Gould, A. Stellar Contribution to the Galactic Bulge Microlensing Optical Depth. ApJ 592, 172–175 (2003). [25] Niikura, H. et al. Microlensing constraints on primordial black holes with Subaru/HSC Andromeda observations. Nature Astronomy 3, 524–534 (2019). [26] Sahu, K. C. Stars within the Large Magellanic Cloud as potential lenses for observed microlensing events. Nature 370, 275–276 (1994). [27] Erkal, D. et al. 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Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. 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[29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. A distance to the Large Magellanic Cloud that is precise to one per cent. Nature 567, 200–203 (2019). [42] Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. An H I Aperture Synthesis Mosaic of the Large Magellanic Cloud. ApJ 503, 674–688 (1998). [44] Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. The dark matter profile of the Milky Way inferred from its circular velocity curve. MNRAS 528, 693–710 (2024). [45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021). Holtzman, J. A., Afonso, C. & Dolphin, A. The Local Group Stellar Populations Archive from the Hubble Space Telescope WFPC2. ApJS 166, 534–548 (2006). [22] Mróz, P. et al. No large population of unbound or wide-orbit Jupiter-mass planets. Nature 548, 183–186 (2017). [23] Cautun, M. et al. The milky way total mass profile as inferred from Gaia DR2. MNRAS 494, 4291–4313 (2020). [24] Han, C. & Gould, A. Stellar Contribution to the Galactic Bulge Microlensing Optical Depth. ApJ 592, 172–175 (2003). [25] Niikura, H. et al. Microlensing constraints on primordial black holes with Subaru/HSC Andromeda observations. Nature Astronomy 3, 524–534 (2019). [26] Sahu, K. C. Stars within the Large Magellanic Cloud as potential lenses for observed microlensing events. Nature 370, 275–276 (1994). [27] Erkal, D. et al. The total mass of the Large Magellanic Cloud from its perturbation on the Orphan stream. MNRAS 487, 2685–2700 (2019). [28] Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. A&A 678, A208 (2023). [29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. 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Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. A distance to the Large Magellanic Cloud that is precise to one per cent. Nature 567, 200–203 (2019). [42] Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. An H I Aperture Synthesis Mosaic of the Large Magellanic Cloud. ApJ 503, 674–688 (1998). [44] Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. The dark matter profile of the Milky Way inferred from its circular velocity curve. MNRAS 528, 693–710 (2024). [45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021). Cautun, M. et al. The milky way total mass profile as inferred from Gaia DR2. MNRAS 494, 4291–4313 (2020). [24] Han, C. & Gould, A. Stellar Contribution to the Galactic Bulge Microlensing Optical Depth. ApJ 592, 172–175 (2003). [25] Niikura, H. et al. Microlensing constraints on primordial black holes with Subaru/HSC Andromeda observations. Nature Astronomy 3, 524–534 (2019). [26] Sahu, K. C. Stars within the Large Magellanic Cloud as potential lenses for observed microlensing events. Nature 370, 275–276 (1994). [27] Erkal, D. et al. The total mass of the Large Magellanic Cloud from its perturbation on the Orphan stream. MNRAS 487, 2685–2700 (2019). [28] Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. A&A 678, A208 (2023). [29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. A distance to the Large Magellanic Cloud that is precise to one per cent. Nature 567, 200–203 (2019). [42] Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. An H I Aperture Synthesis Mosaic of the Large Magellanic Cloud. ApJ 503, 674–688 (1998). [44] Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. The dark matter profile of the Milky Way inferred from its circular velocity curve. MNRAS 528, 693–710 (2024). [45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021). Han, C. & Gould, A. Stellar Contribution to the Galactic Bulge Microlensing Optical Depth. ApJ 592, 172–175 (2003). [25] Niikura, H. et al. Microlensing constraints on primordial black holes with Subaru/HSC Andromeda observations. Nature Astronomy 3, 524–534 (2019). [26] Sahu, K. C. Stars within the Large Magellanic Cloud as potential lenses for observed microlensing events. Nature 370, 275–276 (1994). [27] Erkal, D. et al. The total mass of the Large Magellanic Cloud from its perturbation on the Orphan stream. MNRAS 487, 2685–2700 (2019). [28] Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. A&A 678, A208 (2023). [29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. 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New limits from microlensing on Galactic black holes in the mass range 10 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT < M < 1000 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT. A&A 664, A106 (2022). [19] Udalski, A. The Optical Gravitational Lensing Experiment. Real Time Data Analysis Systems in the OGLE-III Survey. Acta Astron. 53, 291–305 (2003). [20] Mróz, P. et al. Microlensing optical depth and event rate toward the Large Magellanic Cloud based on 20 years of OGLE observations. submitted (2024). [21] Holtzman, J. A., Afonso, C. & Dolphin, A. The Local Group Stellar Populations Archive from the Hubble Space Telescope WFPC2. ApJS 166, 534–548 (2006). [22] Mróz, P. et al. No large population of unbound or wide-orbit Jupiter-mass planets. Nature 548, 183–186 (2017). [23] Cautun, M. et al. The milky way total mass profile as inferred from Gaia DR2. MNRAS 494, 4291–4313 (2020). [24] Han, C. & Gould, A. Stellar Contribution to the Galactic Bulge Microlensing Optical Depth. ApJ 592, 172–175 (2003). [25] Niikura, H. et al. Microlensing constraints on primordial black holes with Subaru/HSC Andromeda observations. Nature Astronomy 3, 524–534 (2019). [26] Sahu, K. C. Stars within the Large Magellanic Cloud as potential lenses for observed microlensing events. Nature 370, 275–276 (1994). [27] Erkal, D. et al. The total mass of the Large Magellanic Cloud from its perturbation on the Orphan stream. MNRAS 487, 2685–2700 (2019). [28] Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. A&A 678, A208 (2023). [29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. A distance to the Large Magellanic Cloud that is precise to one per cent. Nature 567, 200–203 (2019). [42] Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. An H I Aperture Synthesis Mosaic of the Large Magellanic Cloud. ApJ 503, 674–688 (1998). [44] Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. The dark matter profile of the Milky Way inferred from its circular velocity curve. MNRAS 528, 693–710 (2024). [45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021). Escrivà, A., Bagui, E. & Clesse, S. Simulations of PBH formation at the QCD epoch and comparison with the GWTC-3 catalog. J. Cosmology Astropart. Phys 2023, 004 (2023). [13] Udalski, A., Szymański, M. K. & Szymański, G. OGLE-IV: Fourth Phase of the Optical Gravitational Lensing Experiment. Acta Astron. 65, 1–38 (2015). [14] Paczyński, B. Gravitational microlensing by the galactic halo. ApJ 304, 1–5 (1986). [15] Alcock, C. et al. The MACHO Project: Microlensing Results from 5.7 Years of Large Magellanic Cloud Observations. ApJ 542, 281–307 (2000). [16] Tisserand, P. et al. Limits on the Macho content of the Galactic Halo from the EROS-2 Survey of the Magellanic Clouds. A&A 469, 387–404 (2007). [17] Wyrzykowski, L. et al. The OGLE view of microlensing towards the Magellanic Clouds - IV. OGLE-III SMC data and final conclusions on MACHOs. MNRAS 416, 2949–2961 (2011). [18] Blaineau, T. et al. New limits from microlensing on Galactic black holes in the mass range 10 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT < M < 1000 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT. A&A 664, A106 (2022). [19] Udalski, A. The Optical Gravitational Lensing Experiment. Real Time Data Analysis Systems in the OGLE-III Survey. Acta Astron. 53, 291–305 (2003). [20] Mróz, P. et al. Microlensing optical depth and event rate toward the Large Magellanic Cloud based on 20 years of OGLE observations. submitted (2024). [21] Holtzman, J. A., Afonso, C. & Dolphin, A. The Local Group Stellar Populations Archive from the Hubble Space Telescope WFPC2. ApJS 166, 534–548 (2006). [22] Mróz, P. et al. No large population of unbound or wide-orbit Jupiter-mass planets. Nature 548, 183–186 (2017). [23] Cautun, M. et al. The milky way total mass profile as inferred from Gaia DR2. MNRAS 494, 4291–4313 (2020). [24] Han, C. & Gould, A. Stellar Contribution to the Galactic Bulge Microlensing Optical Depth. ApJ 592, 172–175 (2003). [25] Niikura, H. et al. Microlensing constraints on primordial black holes with Subaru/HSC Andromeda observations. Nature Astronomy 3, 524–534 (2019). [26] Sahu, K. C. Stars within the Large Magellanic Cloud as potential lenses for observed microlensing events. Nature 370, 275–276 (1994). [27] Erkal, D. et al. The total mass of the Large Magellanic Cloud from its perturbation on the Orphan stream. MNRAS 487, 2685–2700 (2019). [28] Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. A&A 678, A208 (2023). [29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. A distance to the Large Magellanic Cloud that is precise to one per cent. Nature 567, 200–203 (2019). [42] Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. An H I Aperture Synthesis Mosaic of the Large Magellanic Cloud. ApJ 503, 674–688 (1998). [44] Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. The dark matter profile of the Milky Way inferred from its circular velocity curve. MNRAS 528, 693–710 (2024). [45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021). Udalski, A., Szymański, M. K. & Szymański, G. OGLE-IV: Fourth Phase of the Optical Gravitational Lensing Experiment. Acta Astron. 65, 1–38 (2015). [14] Paczyński, B. Gravitational microlensing by the galactic halo. ApJ 304, 1–5 (1986). [15] Alcock, C. et al. The MACHO Project: Microlensing Results from 5.7 Years of Large Magellanic Cloud Observations. ApJ 542, 281–307 (2000). [16] Tisserand, P. et al. Limits on the Macho content of the Galactic Halo from the EROS-2 Survey of the Magellanic Clouds. A&A 469, 387–404 (2007). [17] Wyrzykowski, L. et al. The OGLE view of microlensing towards the Magellanic Clouds - IV. OGLE-III SMC data and final conclusions on MACHOs. MNRAS 416, 2949–2961 (2011). [18] Blaineau, T. et al. New limits from microlensing on Galactic black holes in the mass range 10 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT < M < 1000 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT. A&A 664, A106 (2022). [19] Udalski, A. The Optical Gravitational Lensing Experiment. Real Time Data Analysis Systems in the OGLE-III Survey. Acta Astron. 53, 291–305 (2003). [20] Mróz, P. et al. Microlensing optical depth and event rate toward the Large Magellanic Cloud based on 20 years of OGLE observations. submitted (2024). [21] Holtzman, J. A., Afonso, C. & Dolphin, A. The Local Group Stellar Populations Archive from the Hubble Space Telescope WFPC2. ApJS 166, 534–548 (2006). [22] Mróz, P. et al. No large population of unbound or wide-orbit Jupiter-mass planets. Nature 548, 183–186 (2017). [23] Cautun, M. et al. The milky way total mass profile as inferred from Gaia DR2. MNRAS 494, 4291–4313 (2020). [24] Han, C. & Gould, A. Stellar Contribution to the Galactic Bulge Microlensing Optical Depth. ApJ 592, 172–175 (2003). [25] Niikura, H. et al. Microlensing constraints on primordial black holes with Subaru/HSC Andromeda observations. Nature Astronomy 3, 524–534 (2019). [26] Sahu, K. C. Stars within the Large Magellanic Cloud as potential lenses for observed microlensing events. Nature 370, 275–276 (1994). [27] Erkal, D. et al. The total mass of the Large Magellanic Cloud from its perturbation on the Orphan stream. MNRAS 487, 2685–2700 (2019). [28] Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. A&A 678, A208 (2023). [29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. A distance to the Large Magellanic Cloud that is precise to one per cent. Nature 567, 200–203 (2019). [42] Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. An H I Aperture Synthesis Mosaic of the Large Magellanic Cloud. ApJ 503, 674–688 (1998). [44] Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. The dark matter profile of the Milky Way inferred from its circular velocity curve. MNRAS 528, 693–710 (2024). [45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021). Paczyński, B. Gravitational microlensing by the galactic halo. ApJ 304, 1–5 (1986). [15] Alcock, C. et al. The MACHO Project: Microlensing Results from 5.7 Years of Large Magellanic Cloud Observations. ApJ 542, 281–307 (2000). [16] Tisserand, P. et al. Limits on the Macho content of the Galactic Halo from the EROS-2 Survey of the Magellanic Clouds. A&A 469, 387–404 (2007). [17] Wyrzykowski, L. et al. The OGLE view of microlensing towards the Magellanic Clouds - IV. OGLE-III SMC data and final conclusions on MACHOs. MNRAS 416, 2949–2961 (2011). [18] Blaineau, T. et al. New limits from microlensing on Galactic black holes in the mass range 10 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT < M < 1000 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT. A&A 664, A106 (2022). [19] Udalski, A. The Optical Gravitational Lensing Experiment. Real Time Data Analysis Systems in the OGLE-III Survey. Acta Astron. 53, 291–305 (2003). [20] Mróz, P. et al. Microlensing optical depth and event rate toward the Large Magellanic Cloud based on 20 years of OGLE observations. submitted (2024). [21] Holtzman, J. A., Afonso, C. & Dolphin, A. The Local Group Stellar Populations Archive from the Hubble Space Telescope WFPC2. ApJS 166, 534–548 (2006). [22] Mróz, P. et al. No large population of unbound or wide-orbit Jupiter-mass planets. Nature 548, 183–186 (2017). [23] Cautun, M. et al. The milky way total mass profile as inferred from Gaia DR2. MNRAS 494, 4291–4313 (2020). [24] Han, C. & Gould, A. Stellar Contribution to the Galactic Bulge Microlensing Optical Depth. ApJ 592, 172–175 (2003). [25] Niikura, H. et al. Microlensing constraints on primordial black holes with Subaru/HSC Andromeda observations. Nature Astronomy 3, 524–534 (2019). [26] Sahu, K. C. Stars within the Large Magellanic Cloud as potential lenses for observed microlensing events. Nature 370, 275–276 (1994). [27] Erkal, D. et al. The total mass of the Large Magellanic Cloud from its perturbation on the Orphan stream. MNRAS 487, 2685–2700 (2019). [28] Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. A&A 678, A208 (2023). [29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. A distance to the Large Magellanic Cloud that is precise to one per cent. Nature 567, 200–203 (2019). [42] Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. An H I Aperture Synthesis Mosaic of the Large Magellanic Cloud. ApJ 503, 674–688 (1998). [44] Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. The dark matter profile of the Milky Way inferred from its circular velocity curve. MNRAS 528, 693–710 (2024). [45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021). Alcock, C. et al. The MACHO Project: Microlensing Results from 5.7 Years of Large Magellanic Cloud Observations. ApJ 542, 281–307 (2000). [16] Tisserand, P. et al. Limits on the Macho content of the Galactic Halo from the EROS-2 Survey of the Magellanic Clouds. A&A 469, 387–404 (2007). [17] Wyrzykowski, L. et al. The OGLE view of microlensing towards the Magellanic Clouds - IV. OGLE-III SMC data and final conclusions on MACHOs. MNRAS 416, 2949–2961 (2011). [18] Blaineau, T. et al. New limits from microlensing on Galactic black holes in the mass range 10 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT < M < 1000 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT. A&A 664, A106 (2022). [19] Udalski, A. The Optical Gravitational Lensing Experiment. Real Time Data Analysis Systems in the OGLE-III Survey. Acta Astron. 53, 291–305 (2003). [20] Mróz, P. et al. Microlensing optical depth and event rate toward the Large Magellanic Cloud based on 20 years of OGLE observations. submitted (2024). [21] Holtzman, J. A., Afonso, C. & Dolphin, A. The Local Group Stellar Populations Archive from the Hubble Space Telescope WFPC2. ApJS 166, 534–548 (2006). [22] Mróz, P. et al. No large population of unbound or wide-orbit Jupiter-mass planets. Nature 548, 183–186 (2017). [23] Cautun, M. et al. The milky way total mass profile as inferred from Gaia DR2. MNRAS 494, 4291–4313 (2020). [24] Han, C. & Gould, A. Stellar Contribution to the Galactic Bulge Microlensing Optical Depth. ApJ 592, 172–175 (2003). [25] Niikura, H. et al. Microlensing constraints on primordial black holes with Subaru/HSC Andromeda observations. Nature Astronomy 3, 524–534 (2019). [26] Sahu, K. C. Stars within the Large Magellanic Cloud as potential lenses for observed microlensing events. Nature 370, 275–276 (1994). [27] Erkal, D. et al. The total mass of the Large Magellanic Cloud from its perturbation on the Orphan stream. MNRAS 487, 2685–2700 (2019). [28] Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. A&A 678, A208 (2023). [29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. A distance to the Large Magellanic Cloud that is precise to one per cent. Nature 567, 200–203 (2019). [42] Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. An H I Aperture Synthesis Mosaic of the Large Magellanic Cloud. ApJ 503, 674–688 (1998). [44] Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. The dark matter profile of the Milky Way inferred from its circular velocity curve. MNRAS 528, 693–710 (2024). [45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021). Tisserand, P. et al. Limits on the Macho content of the Galactic Halo from the EROS-2 Survey of the Magellanic Clouds. A&A 469, 387–404 (2007). [17] Wyrzykowski, L. et al. The OGLE view of microlensing towards the Magellanic Clouds - IV. OGLE-III SMC data and final conclusions on MACHOs. MNRAS 416, 2949–2961 (2011). [18] Blaineau, T. et al. New limits from microlensing on Galactic black holes in the mass range 10 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT < M < 1000 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT. A&A 664, A106 (2022). [19] Udalski, A. The Optical Gravitational Lensing Experiment. Real Time Data Analysis Systems in the OGLE-III Survey. Acta Astron. 53, 291–305 (2003). [20] Mróz, P. et al. Microlensing optical depth and event rate toward the Large Magellanic Cloud based on 20 years of OGLE observations. submitted (2024). [21] Holtzman, J. A., Afonso, C. & Dolphin, A. The Local Group Stellar Populations Archive from the Hubble Space Telescope WFPC2. ApJS 166, 534–548 (2006). [22] Mróz, P. et al. No large population of unbound or wide-orbit Jupiter-mass planets. Nature 548, 183–186 (2017). [23] Cautun, M. et al. The milky way total mass profile as inferred from Gaia DR2. MNRAS 494, 4291–4313 (2020). [24] Han, C. & Gould, A. Stellar Contribution to the Galactic Bulge Microlensing Optical Depth. ApJ 592, 172–175 (2003). [25] Niikura, H. et al. Microlensing constraints on primordial black holes with Subaru/HSC Andromeda observations. Nature Astronomy 3, 524–534 (2019). [26] Sahu, K. C. Stars within the Large Magellanic Cloud as potential lenses for observed microlensing events. Nature 370, 275–276 (1994). [27] Erkal, D. et al. The total mass of the Large Magellanic Cloud from its perturbation on the Orphan stream. MNRAS 487, 2685–2700 (2019). [28] Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. A&A 678, A208 (2023). [29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. A distance to the Large Magellanic Cloud that is precise to one per cent. Nature 567, 200–203 (2019). [42] Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. An H I Aperture Synthesis Mosaic of the Large Magellanic Cloud. ApJ 503, 674–688 (1998). [44] Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. The dark matter profile of the Milky Way inferred from its circular velocity curve. MNRAS 528, 693–710 (2024). [45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021). Wyrzykowski, L. et al. The OGLE view of microlensing towards the Magellanic Clouds - IV. OGLE-III SMC data and final conclusions on MACHOs. MNRAS 416, 2949–2961 (2011). [18] Blaineau, T. et al. New limits from microlensing on Galactic black holes in the mass range 10 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT < M < 1000 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT. A&A 664, A106 (2022). [19] Udalski, A. The Optical Gravitational Lensing Experiment. Real Time Data Analysis Systems in the OGLE-III Survey. Acta Astron. 53, 291–305 (2003). [20] Mróz, P. et al. Microlensing optical depth and event rate toward the Large Magellanic Cloud based on 20 years of OGLE observations. submitted (2024). [21] Holtzman, J. A., Afonso, C. & Dolphin, A. The Local Group Stellar Populations Archive from the Hubble Space Telescope WFPC2. ApJS 166, 534–548 (2006). [22] Mróz, P. et al. No large population of unbound or wide-orbit Jupiter-mass planets. Nature 548, 183–186 (2017). [23] Cautun, M. et al. The milky way total mass profile as inferred from Gaia DR2. MNRAS 494, 4291–4313 (2020). [24] Han, C. & Gould, A. Stellar Contribution to the Galactic Bulge Microlensing Optical Depth. ApJ 592, 172–175 (2003). [25] Niikura, H. et al. Microlensing constraints on primordial black holes with Subaru/HSC Andromeda observations. Nature Astronomy 3, 524–534 (2019). [26] Sahu, K. C. Stars within the Large Magellanic Cloud as potential lenses for observed microlensing events. Nature 370, 275–276 (1994). [27] Erkal, D. et al. The total mass of the Large Magellanic Cloud from its perturbation on the Orphan stream. MNRAS 487, 2685–2700 (2019). [28] Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. A&A 678, A208 (2023). [29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. A distance to the Large Magellanic Cloud that is precise to one per cent. Nature 567, 200–203 (2019). [42] Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. An H I Aperture Synthesis Mosaic of the Large Magellanic Cloud. ApJ 503, 674–688 (1998). [44] Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. The dark matter profile of the Milky Way inferred from its circular velocity curve. MNRAS 528, 693–710 (2024). [45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021). Blaineau, T. et al. New limits from microlensing on Galactic black holes in the mass range 10 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT < M < 1000 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT. A&A 664, A106 (2022). [19] Udalski, A. The Optical Gravitational Lensing Experiment. Real Time Data Analysis Systems in the OGLE-III Survey. Acta Astron. 53, 291–305 (2003). [20] Mróz, P. et al. Microlensing optical depth and event rate toward the Large Magellanic Cloud based on 20 years of OGLE observations. submitted (2024). [21] Holtzman, J. A., Afonso, C. & Dolphin, A. The Local Group Stellar Populations Archive from the Hubble Space Telescope WFPC2. ApJS 166, 534–548 (2006). [22] Mróz, P. et al. No large population of unbound or wide-orbit Jupiter-mass planets. Nature 548, 183–186 (2017). [23] Cautun, M. et al. The milky way total mass profile as inferred from Gaia DR2. MNRAS 494, 4291–4313 (2020). [24] Han, C. & Gould, A. Stellar Contribution to the Galactic Bulge Microlensing Optical Depth. ApJ 592, 172–175 (2003). [25] Niikura, H. et al. Microlensing constraints on primordial black holes with Subaru/HSC Andromeda observations. Nature Astronomy 3, 524–534 (2019). [26] Sahu, K. C. Stars within the Large Magellanic Cloud as potential lenses for observed microlensing events. Nature 370, 275–276 (1994). [27] Erkal, D. et al. The total mass of the Large Magellanic Cloud from its perturbation on the Orphan stream. MNRAS 487, 2685–2700 (2019). [28] Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. A&A 678, A208 (2023). [29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. A distance to the Large Magellanic Cloud that is precise to one per cent. Nature 567, 200–203 (2019). [42] Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. An H I Aperture Synthesis Mosaic of the Large Magellanic Cloud. ApJ 503, 674–688 (1998). [44] Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. The dark matter profile of the Milky Way inferred from its circular velocity curve. MNRAS 528, 693–710 (2024). [45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021). Udalski, A. The Optical Gravitational Lensing Experiment. Real Time Data Analysis Systems in the OGLE-III Survey. Acta Astron. 53, 291–305 (2003). [20] Mróz, P. et al. Microlensing optical depth and event rate toward the Large Magellanic Cloud based on 20 years of OGLE observations. submitted (2024). [21] Holtzman, J. A., Afonso, C. & Dolphin, A. The Local Group Stellar Populations Archive from the Hubble Space Telescope WFPC2. ApJS 166, 534–548 (2006). [22] Mróz, P. et al. No large population of unbound or wide-orbit Jupiter-mass planets. Nature 548, 183–186 (2017). [23] Cautun, M. et al. The milky way total mass profile as inferred from Gaia DR2. MNRAS 494, 4291–4313 (2020). [24] Han, C. & Gould, A. Stellar Contribution to the Galactic Bulge Microlensing Optical Depth. ApJ 592, 172–175 (2003). [25] Niikura, H. et al. Microlensing constraints on primordial black holes with Subaru/HSC Andromeda observations. Nature Astronomy 3, 524–534 (2019). [26] Sahu, K. C. Stars within the Large Magellanic Cloud as potential lenses for observed microlensing events. Nature 370, 275–276 (1994). [27] Erkal, D. et al. The total mass of the Large Magellanic Cloud from its perturbation on the Orphan stream. MNRAS 487, 2685–2700 (2019). [28] Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. A&A 678, A208 (2023). [29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. A distance to the Large Magellanic Cloud that is precise to one per cent. Nature 567, 200–203 (2019). [42] Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. An H I Aperture Synthesis Mosaic of the Large Magellanic Cloud. ApJ 503, 674–688 (1998). [44] Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. The dark matter profile of the Milky Way inferred from its circular velocity curve. MNRAS 528, 693–710 (2024). [45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021). Mróz, P. et al. Microlensing optical depth and event rate toward the Large Magellanic Cloud based on 20 years of OGLE observations. submitted (2024). [21] Holtzman, J. A., Afonso, C. & Dolphin, A. The Local Group Stellar Populations Archive from the Hubble Space Telescope WFPC2. ApJS 166, 534–548 (2006). [22] Mróz, P. et al. No large population of unbound or wide-orbit Jupiter-mass planets. Nature 548, 183–186 (2017). [23] Cautun, M. et al. The milky way total mass profile as inferred from Gaia DR2. MNRAS 494, 4291–4313 (2020). [24] Han, C. & Gould, A. Stellar Contribution to the Galactic Bulge Microlensing Optical Depth. ApJ 592, 172–175 (2003). [25] Niikura, H. et al. Microlensing constraints on primordial black holes with Subaru/HSC Andromeda observations. Nature Astronomy 3, 524–534 (2019). [26] Sahu, K. C. Stars within the Large Magellanic Cloud as potential lenses for observed microlensing events. Nature 370, 275–276 (1994). [27] Erkal, D. et al. The total mass of the Large Magellanic Cloud from its perturbation on the Orphan stream. MNRAS 487, 2685–2700 (2019). [28] Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. A&A 678, A208 (2023). [29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. A distance to the Large Magellanic Cloud that is precise to one per cent. Nature 567, 200–203 (2019). [42] Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. An H I Aperture Synthesis Mosaic of the Large Magellanic Cloud. ApJ 503, 674–688 (1998). [44] Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. The dark matter profile of the Milky Way inferred from its circular velocity curve. MNRAS 528, 693–710 (2024). [45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021). Holtzman, J. A., Afonso, C. & Dolphin, A. The Local Group Stellar Populations Archive from the Hubble Space Telescope WFPC2. ApJS 166, 534–548 (2006). [22] Mróz, P. et al. No large population of unbound or wide-orbit Jupiter-mass planets. Nature 548, 183–186 (2017). [23] Cautun, M. et al. The milky way total mass profile as inferred from Gaia DR2. MNRAS 494, 4291–4313 (2020). [24] Han, C. & Gould, A. Stellar Contribution to the Galactic Bulge Microlensing Optical Depth. ApJ 592, 172–175 (2003). [25] Niikura, H. et al. Microlensing constraints on primordial black holes with Subaru/HSC Andromeda observations. Nature Astronomy 3, 524–534 (2019). [26] Sahu, K. C. Stars within the Large Magellanic Cloud as potential lenses for observed microlensing events. Nature 370, 275–276 (1994). [27] Erkal, D. et al. The total mass of the Large Magellanic Cloud from its perturbation on the Orphan stream. MNRAS 487, 2685–2700 (2019). [28] Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. A&A 678, A208 (2023). [29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). 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The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. A distance to the Large Magellanic Cloud that is precise to one per cent. Nature 567, 200–203 (2019). [42] Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. An H I Aperture Synthesis Mosaic of the Large Magellanic Cloud. ApJ 503, 674–688 (1998). [44] Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. The dark matter profile of the Milky Way inferred from its circular velocity curve. MNRAS 528, 693–710 (2024). [45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021). Jedamzik, K. Consistency of Primordial Black Hole Dark Matter with LIGO/Virgo Merger Rates. Phys. Rev. Lett. 126, 051302 (2021). [12] Escrivà, A., Bagui, E. & Clesse, S. Simulations of PBH formation at the QCD epoch and comparison with the GWTC-3 catalog. J. Cosmology Astropart. Phys 2023, 004 (2023). [13] Udalski, A., Szymański, M. K. & Szymański, G. OGLE-IV: Fourth Phase of the Optical Gravitational Lensing Experiment. Acta Astron. 65, 1–38 (2015). [14] Paczyński, B. Gravitational microlensing by the galactic halo. ApJ 304, 1–5 (1986). [15] Alcock, C. et al. The MACHO Project: Microlensing Results from 5.7 Years of Large Magellanic Cloud Observations. ApJ 542, 281–307 (2000). [16] Tisserand, P. et al. Limits on the Macho content of the Galactic Halo from the EROS-2 Survey of the Magellanic Clouds. A&A 469, 387–404 (2007). [17] Wyrzykowski, L. et al. The OGLE view of microlensing towards the Magellanic Clouds - IV. OGLE-III SMC data and final conclusions on MACHOs. MNRAS 416, 2949–2961 (2011). [18] Blaineau, T. et al. New limits from microlensing on Galactic black holes in the mass range 10 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT < M < 1000 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT. A&A 664, A106 (2022). [19] Udalski, A. The Optical Gravitational Lensing Experiment. Real Time Data Analysis Systems in the OGLE-III Survey. Acta Astron. 53, 291–305 (2003). [20] Mróz, P. et al. Microlensing optical depth and event rate toward the Large Magellanic Cloud based on 20 years of OGLE observations. submitted (2024). [21] Holtzman, J. A., Afonso, C. & Dolphin, A. The Local Group Stellar Populations Archive from the Hubble Space Telescope WFPC2. ApJS 166, 534–548 (2006). [22] Mróz, P. et al. No large population of unbound or wide-orbit Jupiter-mass planets. Nature 548, 183–186 (2017). [23] Cautun, M. et al. The milky way total mass profile as inferred from Gaia DR2. MNRAS 494, 4291–4313 (2020). [24] Han, C. & Gould, A. Stellar Contribution to the Galactic Bulge Microlensing Optical Depth. ApJ 592, 172–175 (2003). [25] Niikura, H. et al. Microlensing constraints on primordial black holes with Subaru/HSC Andromeda observations. Nature Astronomy 3, 524–534 (2019). [26] Sahu, K. C. Stars within the Large Magellanic Cloud as potential lenses for observed microlensing events. Nature 370, 275–276 (1994). [27] Erkal, D. et al. The total mass of the Large Magellanic Cloud from its perturbation on the Orphan stream. MNRAS 487, 2685–2700 (2019). [28] Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. A&A 678, A208 (2023). [29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. A distance to the Large Magellanic Cloud that is precise to one per cent. Nature 567, 200–203 (2019). [42] Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. An H I Aperture Synthesis Mosaic of the Large Magellanic Cloud. ApJ 503, 674–688 (1998). [44] Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. The dark matter profile of the Milky Way inferred from its circular velocity curve. MNRAS 528, 693–710 (2024). [45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021). Escrivà, A., Bagui, E. & Clesse, S. Simulations of PBH formation at the QCD epoch and comparison with the GWTC-3 catalog. J. Cosmology Astropart. Phys 2023, 004 (2023). [13] Udalski, A., Szymański, M. K. & Szymański, G. OGLE-IV: Fourth Phase of the Optical Gravitational Lensing Experiment. Acta Astron. 65, 1–38 (2015). [14] Paczyński, B. Gravitational microlensing by the galactic halo. ApJ 304, 1–5 (1986). [15] Alcock, C. et al. The MACHO Project: Microlensing Results from 5.7 Years of Large Magellanic Cloud Observations. ApJ 542, 281–307 (2000). [16] Tisserand, P. et al. Limits on the Macho content of the Galactic Halo from the EROS-2 Survey of the Magellanic Clouds. A&A 469, 387–404 (2007). [17] Wyrzykowski, L. et al. The OGLE view of microlensing towards the Magellanic Clouds - IV. OGLE-III SMC data and final conclusions on MACHOs. MNRAS 416, 2949–2961 (2011). [18] Blaineau, T. et al. New limits from microlensing on Galactic black holes in the mass range 10 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT < M < 1000 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT. A&A 664, A106 (2022). [19] Udalski, A. The Optical Gravitational Lensing Experiment. Real Time Data Analysis Systems in the OGLE-III Survey. Acta Astron. 53, 291–305 (2003). [20] Mróz, P. et al. Microlensing optical depth and event rate toward the Large Magellanic Cloud based on 20 years of OGLE observations. submitted (2024). [21] Holtzman, J. A., Afonso, C. & Dolphin, A. The Local Group Stellar Populations Archive from the Hubble Space Telescope WFPC2. ApJS 166, 534–548 (2006). [22] Mróz, P. et al. No large population of unbound or wide-orbit Jupiter-mass planets. Nature 548, 183–186 (2017). [23] Cautun, M. et al. The milky way total mass profile as inferred from Gaia DR2. MNRAS 494, 4291–4313 (2020). [24] Han, C. & Gould, A. Stellar Contribution to the Galactic Bulge Microlensing Optical Depth. ApJ 592, 172–175 (2003). [25] Niikura, H. et al. Microlensing constraints on primordial black holes with Subaru/HSC Andromeda observations. Nature Astronomy 3, 524–534 (2019). [26] Sahu, K. C. Stars within the Large Magellanic Cloud as potential lenses for observed microlensing events. Nature 370, 275–276 (1994). [27] Erkal, D. et al. The total mass of the Large Magellanic Cloud from its perturbation on the Orphan stream. MNRAS 487, 2685–2700 (2019). [28] Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. A&A 678, A208 (2023). [29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. A distance to the Large Magellanic Cloud that is precise to one per cent. Nature 567, 200–203 (2019). [42] Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. An H I Aperture Synthesis Mosaic of the Large Magellanic Cloud. ApJ 503, 674–688 (1998). [44] Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. The dark matter profile of the Milky Way inferred from its circular velocity curve. MNRAS 528, 693–710 (2024). [45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021). Udalski, A., Szymański, M. K. & Szymański, G. OGLE-IV: Fourth Phase of the Optical Gravitational Lensing Experiment. Acta Astron. 65, 1–38 (2015). [14] Paczyński, B. Gravitational microlensing by the galactic halo. ApJ 304, 1–5 (1986). [15] Alcock, C. et al. The MACHO Project: Microlensing Results from 5.7 Years of Large Magellanic Cloud Observations. ApJ 542, 281–307 (2000). [16] Tisserand, P. et al. Limits on the Macho content of the Galactic Halo from the EROS-2 Survey of the Magellanic Clouds. A&A 469, 387–404 (2007). [17] Wyrzykowski, L. et al. The OGLE view of microlensing towards the Magellanic Clouds - IV. OGLE-III SMC data and final conclusions on MACHOs. MNRAS 416, 2949–2961 (2011). [18] Blaineau, T. et al. New limits from microlensing on Galactic black holes in the mass range 10 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT < M < 1000 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT. A&A 664, A106 (2022). [19] Udalski, A. The Optical Gravitational Lensing Experiment. Real Time Data Analysis Systems in the OGLE-III Survey. Acta Astron. 53, 291–305 (2003). [20] Mróz, P. et al. Microlensing optical depth and event rate toward the Large Magellanic Cloud based on 20 years of OGLE observations. submitted (2024). [21] Holtzman, J. A., Afonso, C. & Dolphin, A. The Local Group Stellar Populations Archive from the Hubble Space Telescope WFPC2. ApJS 166, 534–548 (2006). [22] Mróz, P. et al. No large population of unbound or wide-orbit Jupiter-mass planets. Nature 548, 183–186 (2017). [23] Cautun, M. et al. The milky way total mass profile as inferred from Gaia DR2. MNRAS 494, 4291–4313 (2020). [24] Han, C. & Gould, A. Stellar Contribution to the Galactic Bulge Microlensing Optical Depth. ApJ 592, 172–175 (2003). [25] Niikura, H. et al. Microlensing constraints on primordial black holes with Subaru/HSC Andromeda observations. Nature Astronomy 3, 524–534 (2019). [26] Sahu, K. C. Stars within the Large Magellanic Cloud as potential lenses for observed microlensing events. Nature 370, 275–276 (1994). [27] Erkal, D. et al. The total mass of the Large Magellanic Cloud from its perturbation on the Orphan stream. MNRAS 487, 2685–2700 (2019). [28] Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. A&A 678, A208 (2023). [29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. A distance to the Large Magellanic Cloud that is precise to one per cent. Nature 567, 200–203 (2019). [42] Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. An H I Aperture Synthesis Mosaic of the Large Magellanic Cloud. ApJ 503, 674–688 (1998). [44] Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. The dark matter profile of the Milky Way inferred from its circular velocity curve. MNRAS 528, 693–710 (2024). [45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021). Paczyński, B. Gravitational microlensing by the galactic halo. ApJ 304, 1–5 (1986). [15] Alcock, C. et al. The MACHO Project: Microlensing Results from 5.7 Years of Large Magellanic Cloud Observations. ApJ 542, 281–307 (2000). [16] Tisserand, P. et al. Limits on the Macho content of the Galactic Halo from the EROS-2 Survey of the Magellanic Clouds. A&A 469, 387–404 (2007). [17] Wyrzykowski, L. et al. The OGLE view of microlensing towards the Magellanic Clouds - IV. OGLE-III SMC data and final conclusions on MACHOs. MNRAS 416, 2949–2961 (2011). [18] Blaineau, T. et al. New limits from microlensing on Galactic black holes in the mass range 10 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT < M < 1000 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT. A&A 664, A106 (2022). [19] Udalski, A. The Optical Gravitational Lensing Experiment. Real Time Data Analysis Systems in the OGLE-III Survey. Acta Astron. 53, 291–305 (2003). [20] Mróz, P. et al. Microlensing optical depth and event rate toward the Large Magellanic Cloud based on 20 years of OGLE observations. submitted (2024). [21] Holtzman, J. A., Afonso, C. & Dolphin, A. The Local Group Stellar Populations Archive from the Hubble Space Telescope WFPC2. ApJS 166, 534–548 (2006). [22] Mróz, P. et al. No large population of unbound or wide-orbit Jupiter-mass planets. Nature 548, 183–186 (2017). [23] Cautun, M. et al. The milky way total mass profile as inferred from Gaia DR2. MNRAS 494, 4291–4313 (2020). [24] Han, C. & Gould, A. Stellar Contribution to the Galactic Bulge Microlensing Optical Depth. ApJ 592, 172–175 (2003). [25] Niikura, H. et al. Microlensing constraints on primordial black holes with Subaru/HSC Andromeda observations. Nature Astronomy 3, 524–534 (2019). [26] Sahu, K. C. Stars within the Large Magellanic Cloud as potential lenses for observed microlensing events. Nature 370, 275–276 (1994). [27] Erkal, D. et al. The total mass of the Large Magellanic Cloud from its perturbation on the Orphan stream. MNRAS 487, 2685–2700 (2019). [28] Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. A&A 678, A208 (2023). [29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. A distance to the Large Magellanic Cloud that is precise to one per cent. Nature 567, 200–203 (2019). [42] Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. An H I Aperture Synthesis Mosaic of the Large Magellanic Cloud. ApJ 503, 674–688 (1998). [44] Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. The dark matter profile of the Milky Way inferred from its circular velocity curve. MNRAS 528, 693–710 (2024). [45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021). Alcock, C. et al. The MACHO Project: Microlensing Results from 5.7 Years of Large Magellanic Cloud Observations. ApJ 542, 281–307 (2000). [16] Tisserand, P. et al. Limits on the Macho content of the Galactic Halo from the EROS-2 Survey of the Magellanic Clouds. A&A 469, 387–404 (2007). [17] Wyrzykowski, L. et al. The OGLE view of microlensing towards the Magellanic Clouds - IV. OGLE-III SMC data and final conclusions on MACHOs. MNRAS 416, 2949–2961 (2011). [18] Blaineau, T. et al. New limits from microlensing on Galactic black holes in the mass range 10 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT < M < 1000 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT. A&A 664, A106 (2022). [19] Udalski, A. The Optical Gravitational Lensing Experiment. Real Time Data Analysis Systems in the OGLE-III Survey. Acta Astron. 53, 291–305 (2003). [20] Mróz, P. et al. Microlensing optical depth and event rate toward the Large Magellanic Cloud based on 20 years of OGLE observations. submitted (2024). [21] Holtzman, J. A., Afonso, C. & Dolphin, A. The Local Group Stellar Populations Archive from the Hubble Space Telescope WFPC2. ApJS 166, 534–548 (2006). [22] Mróz, P. et al. No large population of unbound or wide-orbit Jupiter-mass planets. Nature 548, 183–186 (2017). [23] Cautun, M. et al. The milky way total mass profile as inferred from Gaia DR2. MNRAS 494, 4291–4313 (2020). [24] Han, C. & Gould, A. Stellar Contribution to the Galactic Bulge Microlensing Optical Depth. ApJ 592, 172–175 (2003). [25] Niikura, H. et al. Microlensing constraints on primordial black holes with Subaru/HSC Andromeda observations. Nature Astronomy 3, 524–534 (2019). [26] Sahu, K. C. Stars within the Large Magellanic Cloud as potential lenses for observed microlensing events. Nature 370, 275–276 (1994). [27] Erkal, D. et al. The total mass of the Large Magellanic Cloud from its perturbation on the Orphan stream. MNRAS 487, 2685–2700 (2019). [28] Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. A&A 678, A208 (2023). [29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. 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Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021). Tisserand, P. et al. Limits on the Macho content of the Galactic Halo from the EROS-2 Survey of the Magellanic Clouds. A&A 469, 387–404 (2007). [17] Wyrzykowski, L. et al. The OGLE view of microlensing towards the Magellanic Clouds - IV. OGLE-III SMC data and final conclusions on MACHOs. MNRAS 416, 2949–2961 (2011). [18] Blaineau, T. et al. New limits from microlensing on Galactic black holes in the mass range 10 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT < M < 1000 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT. A&A 664, A106 (2022). [19] Udalski, A. The Optical Gravitational Lensing Experiment. Real Time Data Analysis Systems in the OGLE-III Survey. Acta Astron. 53, 291–305 (2003). [20] Mróz, P. et al. Microlensing optical depth and event rate toward the Large Magellanic Cloud based on 20 years of OGLE observations. submitted (2024). [21] Holtzman, J. A., Afonso, C. & Dolphin, A. The Local Group Stellar Populations Archive from the Hubble Space Telescope WFPC2. ApJS 166, 534–548 (2006). [22] Mróz, P. et al. No large population of unbound or wide-orbit Jupiter-mass planets. Nature 548, 183–186 (2017). [23] Cautun, M. et al. The milky way total mass profile as inferred from Gaia DR2. MNRAS 494, 4291–4313 (2020). [24] Han, C. & Gould, A. Stellar Contribution to the Galactic Bulge Microlensing Optical Depth. ApJ 592, 172–175 (2003). [25] Niikura, H. et al. Microlensing constraints on primordial black holes with Subaru/HSC Andromeda observations. Nature Astronomy 3, 524–534 (2019). [26] Sahu, K. C. Stars within the Large Magellanic Cloud as potential lenses for observed microlensing events. Nature 370, 275–276 (1994). [27] Erkal, D. et al. The total mass of the Large Magellanic Cloud from its perturbation on the Orphan stream. MNRAS 487, 2685–2700 (2019). [28] Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. A&A 678, A208 (2023). [29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. A distance to the Large Magellanic Cloud that is precise to one per cent. Nature 567, 200–203 (2019). [42] Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. An H I Aperture Synthesis Mosaic of the Large Magellanic Cloud. ApJ 503, 674–688 (1998). [44] Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. The dark matter profile of the Milky Way inferred from its circular velocity curve. MNRAS 528, 693–710 (2024). [45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021). Wyrzykowski, L. et al. The OGLE view of microlensing towards the Magellanic Clouds - IV. OGLE-III SMC data and final conclusions on MACHOs. MNRAS 416, 2949–2961 (2011). [18] Blaineau, T. et al. New limits from microlensing on Galactic black holes in the mass range 10 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT < M < 1000 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT. A&A 664, A106 (2022). [19] Udalski, A. The Optical Gravitational Lensing Experiment. Real Time Data Analysis Systems in the OGLE-III Survey. Acta Astron. 53, 291–305 (2003). [20] Mróz, P. et al. Microlensing optical depth and event rate toward the Large Magellanic Cloud based on 20 years of OGLE observations. submitted (2024). [21] Holtzman, J. A., Afonso, C. & Dolphin, A. The Local Group Stellar Populations Archive from the Hubble Space Telescope WFPC2. ApJS 166, 534–548 (2006). [22] Mróz, P. et al. No large population of unbound or wide-orbit Jupiter-mass planets. Nature 548, 183–186 (2017). [23] Cautun, M. et al. The milky way total mass profile as inferred from Gaia DR2. MNRAS 494, 4291–4313 (2020). [24] Han, C. & Gould, A. Stellar Contribution to the Galactic Bulge Microlensing Optical Depth. ApJ 592, 172–175 (2003). [25] Niikura, H. et al. Microlensing constraints on primordial black holes with Subaru/HSC Andromeda observations. Nature Astronomy 3, 524–534 (2019). [26] Sahu, K. C. Stars within the Large Magellanic Cloud as potential lenses for observed microlensing events. Nature 370, 275–276 (1994). [27] Erkal, D. et al. The total mass of the Large Magellanic Cloud from its perturbation on the Orphan stream. MNRAS 487, 2685–2700 (2019). [28] Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. A&A 678, A208 (2023). [29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. A distance to the Large Magellanic Cloud that is precise to one per cent. Nature 567, 200–203 (2019). [42] Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. An H I Aperture Synthesis Mosaic of the Large Magellanic Cloud. ApJ 503, 674–688 (1998). [44] Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. The dark matter profile of the Milky Way inferred from its circular velocity curve. MNRAS 528, 693–710 (2024). [45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021). Blaineau, T. et al. New limits from microlensing on Galactic black holes in the mass range 10 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT < M < 1000 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT. A&A 664, A106 (2022). [19] Udalski, A. The Optical Gravitational Lensing Experiment. Real Time Data Analysis Systems in the OGLE-III Survey. Acta Astron. 53, 291–305 (2003). [20] Mróz, P. et al. Microlensing optical depth and event rate toward the Large Magellanic Cloud based on 20 years of OGLE observations. submitted (2024). [21] Holtzman, J. A., Afonso, C. & Dolphin, A. The Local Group Stellar Populations Archive from the Hubble Space Telescope WFPC2. ApJS 166, 534–548 (2006). [22] Mróz, P. et al. No large population of unbound or wide-orbit Jupiter-mass planets. Nature 548, 183–186 (2017). [23] Cautun, M. et al. The milky way total mass profile as inferred from Gaia DR2. MNRAS 494, 4291–4313 (2020). [24] Han, C. & Gould, A. Stellar Contribution to the Galactic Bulge Microlensing Optical Depth. ApJ 592, 172–175 (2003). [25] Niikura, H. et al. Microlensing constraints on primordial black holes with Subaru/HSC Andromeda observations. Nature Astronomy 3, 524–534 (2019). [26] Sahu, K. C. Stars within the Large Magellanic Cloud as potential lenses for observed microlensing events. Nature 370, 275–276 (1994). [27] Erkal, D. et al. The total mass of the Large Magellanic Cloud from its perturbation on the Orphan stream. MNRAS 487, 2685–2700 (2019). [28] Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. A&A 678, A208 (2023). [29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. A distance to the Large Magellanic Cloud that is precise to one per cent. Nature 567, 200–203 (2019). [42] Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. An H I Aperture Synthesis Mosaic of the Large Magellanic Cloud. ApJ 503, 674–688 (1998). [44] Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. The dark matter profile of the Milky Way inferred from its circular velocity curve. MNRAS 528, 693–710 (2024). [45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021). Udalski, A. The Optical Gravitational Lensing Experiment. Real Time Data Analysis Systems in the OGLE-III Survey. Acta Astron. 53, 291–305 (2003). [20] Mróz, P. et al. Microlensing optical depth and event rate toward the Large Magellanic Cloud based on 20 years of OGLE observations. submitted (2024). [21] Holtzman, J. A., Afonso, C. & Dolphin, A. The Local Group Stellar Populations Archive from the Hubble Space Telescope WFPC2. ApJS 166, 534–548 (2006). [22] Mróz, P. et al. No large population of unbound or wide-orbit Jupiter-mass planets. Nature 548, 183–186 (2017). [23] Cautun, M. et al. The milky way total mass profile as inferred from Gaia DR2. MNRAS 494, 4291–4313 (2020). [24] Han, C. & Gould, A. Stellar Contribution to the Galactic Bulge Microlensing Optical Depth. ApJ 592, 172–175 (2003). [25] Niikura, H. et al. Microlensing constraints on primordial black holes with Subaru/HSC Andromeda observations. Nature Astronomy 3, 524–534 (2019). [26] Sahu, K. C. Stars within the Large Magellanic Cloud as potential lenses for observed microlensing events. Nature 370, 275–276 (1994). [27] Erkal, D. et al. The total mass of the Large Magellanic Cloud from its perturbation on the Orphan stream. MNRAS 487, 2685–2700 (2019). [28] Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. A&A 678, A208 (2023). [29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. A distance to the Large Magellanic Cloud that is precise to one per cent. Nature 567, 200–203 (2019). [42] Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. An H I Aperture Synthesis Mosaic of the Large Magellanic Cloud. ApJ 503, 674–688 (1998). [44] Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. The dark matter profile of the Milky Way inferred from its circular velocity curve. MNRAS 528, 693–710 (2024). [45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021). Mróz, P. et al. Microlensing optical depth and event rate toward the Large Magellanic Cloud based on 20 years of OGLE observations. submitted (2024). [21] Holtzman, J. A., Afonso, C. & Dolphin, A. The Local Group Stellar Populations Archive from the Hubble Space Telescope WFPC2. ApJS 166, 534–548 (2006). [22] Mróz, P. et al. No large population of unbound or wide-orbit Jupiter-mass planets. Nature 548, 183–186 (2017). [23] Cautun, M. et al. The milky way total mass profile as inferred from Gaia DR2. MNRAS 494, 4291–4313 (2020). [24] Han, C. & Gould, A. Stellar Contribution to the Galactic Bulge Microlensing Optical Depth. ApJ 592, 172–175 (2003). [25] Niikura, H. et al. Microlensing constraints on primordial black holes with Subaru/HSC Andromeda observations. Nature Astronomy 3, 524–534 (2019). [26] Sahu, K. C. Stars within the Large Magellanic Cloud as potential lenses for observed microlensing events. Nature 370, 275–276 (1994). [27] Erkal, D. et al. The total mass of the Large Magellanic Cloud from its perturbation on the Orphan stream. MNRAS 487, 2685–2700 (2019). [28] Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. A&A 678, A208 (2023). [29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. A distance to the Large Magellanic Cloud that is precise to one per cent. Nature 567, 200–203 (2019). [42] Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. An H I Aperture Synthesis Mosaic of the Large Magellanic Cloud. ApJ 503, 674–688 (1998). [44] Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. The dark matter profile of the Milky Way inferred from its circular velocity curve. MNRAS 528, 693–710 (2024). [45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. 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[29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). 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The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. 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The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. 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New limits from microlensing on Galactic black holes in the mass range 10 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT < M < 1000 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT. A&A 664, A106 (2022). [19] Udalski, A. The Optical Gravitational Lensing Experiment. Real Time Data Analysis Systems in the OGLE-III Survey. Acta Astron. 53, 291–305 (2003). [20] Mróz, P. et al. Microlensing optical depth and event rate toward the Large Magellanic Cloud based on 20 years of OGLE observations. submitted (2024). [21] Holtzman, J. A., Afonso, C. & Dolphin, A. The Local Group Stellar Populations Archive from the Hubble Space Telescope WFPC2. ApJS 166, 534–548 (2006). [22] Mróz, P. et al. No large population of unbound or wide-orbit Jupiter-mass planets. Nature 548, 183–186 (2017). [23] Cautun, M. et al. The milky way total mass profile as inferred from Gaia DR2. MNRAS 494, 4291–4313 (2020). [24] Han, C. & Gould, A. Stellar Contribution to the Galactic Bulge Microlensing Optical Depth. ApJ 592, 172–175 (2003). [25] Niikura, H. et al. Microlensing constraints on primordial black holes with Subaru/HSC Andromeda observations. Nature Astronomy 3, 524–534 (2019). [26] Sahu, K. C. Stars within the Large Magellanic Cloud as potential lenses for observed microlensing events. Nature 370, 275–276 (1994). [27] Erkal, D. et al. The total mass of the Large Magellanic Cloud from its perturbation on the Orphan stream. MNRAS 487, 2685–2700 (2019). [28] Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. A&A 678, A208 (2023). [29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. 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A&A 664, A106 (2022). [19] Udalski, A. The Optical Gravitational Lensing Experiment. Real Time Data Analysis Systems in the OGLE-III Survey. Acta Astron. 53, 291–305 (2003). [20] Mróz, P. et al. Microlensing optical depth and event rate toward the Large Magellanic Cloud based on 20 years of OGLE observations. submitted (2024). [21] Holtzman, J. A., Afonso, C. & Dolphin, A. The Local Group Stellar Populations Archive from the Hubble Space Telescope WFPC2. ApJS 166, 534–548 (2006). [22] Mróz, P. et al. No large population of unbound or wide-orbit Jupiter-mass planets. Nature 548, 183–186 (2017). [23] Cautun, M. et al. The milky way total mass profile as inferred from Gaia DR2. MNRAS 494, 4291–4313 (2020). [24] Han, C. & Gould, A. Stellar Contribution to the Galactic Bulge Microlensing Optical Depth. ApJ 592, 172–175 (2003). [25] Niikura, H. et al. Microlensing constraints on primordial black holes with Subaru/HSC Andromeda observations. Nature Astronomy 3, 524–534 (2019). [26] Sahu, K. C. Stars within the Large Magellanic Cloud as potential lenses for observed microlensing events. Nature 370, 275–276 (1994). [27] Erkal, D. et al. The total mass of the Large Magellanic Cloud from its perturbation on the Orphan stream. MNRAS 487, 2685–2700 (2019). [28] Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. A&A 678, A208 (2023). [29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. A distance to the Large Magellanic Cloud that is precise to one per cent. Nature 567, 200–203 (2019). [42] Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. An H I Aperture Synthesis Mosaic of the Large Magellanic Cloud. ApJ 503, 674–688 (1998). [44] Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. The dark matter profile of the Milky Way inferred from its circular velocity curve. MNRAS 528, 693–710 (2024). [45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021). Alcock, C. et al. The MACHO Project: Microlensing Results from 5.7 Years of Large Magellanic Cloud Observations. ApJ 542, 281–307 (2000). [16] Tisserand, P. et al. Limits on the Macho content of the Galactic Halo from the EROS-2 Survey of the Magellanic Clouds. A&A 469, 387–404 (2007). [17] Wyrzykowski, L. et al. The OGLE view of microlensing towards the Magellanic Clouds - IV. OGLE-III SMC data and final conclusions on MACHOs. MNRAS 416, 2949–2961 (2011). [18] Blaineau, T. et al. New limits from microlensing on Galactic black holes in the mass range 10 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT < M < 1000 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT. A&A 664, A106 (2022). [19] Udalski, A. The Optical Gravitational Lensing Experiment. Real Time Data Analysis Systems in the OGLE-III Survey. Acta Astron. 53, 291–305 (2003). [20] Mróz, P. et al. Microlensing optical depth and event rate toward the Large Magellanic Cloud based on 20 years of OGLE observations. submitted (2024). [21] Holtzman, J. A., Afonso, C. & Dolphin, A. The Local Group Stellar Populations Archive from the Hubble Space Telescope WFPC2. ApJS 166, 534–548 (2006). [22] Mróz, P. et al. No large population of unbound or wide-orbit Jupiter-mass planets. Nature 548, 183–186 (2017). [23] Cautun, M. et al. The milky way total mass profile as inferred from Gaia DR2. MNRAS 494, 4291–4313 (2020). [24] Han, C. & Gould, A. Stellar Contribution to the Galactic Bulge Microlensing Optical Depth. ApJ 592, 172–175 (2003). [25] Niikura, H. et al. Microlensing constraints on primordial black holes with Subaru/HSC Andromeda observations. Nature Astronomy 3, 524–534 (2019). [26] Sahu, K. C. Stars within the Large Magellanic Cloud as potential lenses for observed microlensing events. Nature 370, 275–276 (1994). [27] Erkal, D. et al. The total mass of the Large Magellanic Cloud from its perturbation on the Orphan stream. MNRAS 487, 2685–2700 (2019). [28] Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. A&A 678, A208 (2023). [29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. A distance to the Large Magellanic Cloud that is precise to one per cent. Nature 567, 200–203 (2019). [42] Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. An H I Aperture Synthesis Mosaic of the Large Magellanic Cloud. ApJ 503, 674–688 (1998). [44] Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. The dark matter profile of the Milky Way inferred from its circular velocity curve. MNRAS 528, 693–710 (2024). [45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021). Tisserand, P. et al. Limits on the Macho content of the Galactic Halo from the EROS-2 Survey of the Magellanic Clouds. A&A 469, 387–404 (2007). [17] Wyrzykowski, L. et al. The OGLE view of microlensing towards the Magellanic Clouds - IV. OGLE-III SMC data and final conclusions on MACHOs. MNRAS 416, 2949–2961 (2011). [18] Blaineau, T. et al. New limits from microlensing on Galactic black holes in the mass range 10 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT < M < 1000 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT. A&A 664, A106 (2022). [19] Udalski, A. The Optical Gravitational Lensing Experiment. Real Time Data Analysis Systems in the OGLE-III Survey. Acta Astron. 53, 291–305 (2003). [20] Mróz, P. et al. Microlensing optical depth and event rate toward the Large Magellanic Cloud based on 20 years of OGLE observations. submitted (2024). [21] Holtzman, J. A., Afonso, C. & Dolphin, A. The Local Group Stellar Populations Archive from the Hubble Space Telescope WFPC2. ApJS 166, 534–548 (2006). [22] Mróz, P. et al. No large population of unbound or wide-orbit Jupiter-mass planets. Nature 548, 183–186 (2017). [23] Cautun, M. et al. The milky way total mass profile as inferred from Gaia DR2. MNRAS 494, 4291–4313 (2020). [24] Han, C. & Gould, A. Stellar Contribution to the Galactic Bulge Microlensing Optical Depth. ApJ 592, 172–175 (2003). [25] Niikura, H. et al. Microlensing constraints on primordial black holes with Subaru/HSC Andromeda observations. Nature Astronomy 3, 524–534 (2019). [26] Sahu, K. C. Stars within the Large Magellanic Cloud as potential lenses for observed microlensing events. Nature 370, 275–276 (1994). [27] Erkal, D. et al. The total mass of the Large Magellanic Cloud from its perturbation on the Orphan stream. MNRAS 487, 2685–2700 (2019). [28] Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. A&A 678, A208 (2023). [29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. A distance to the Large Magellanic Cloud that is precise to one per cent. Nature 567, 200–203 (2019). [42] Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. An H I Aperture Synthesis Mosaic of the Large Magellanic Cloud. ApJ 503, 674–688 (1998). [44] Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. The dark matter profile of the Milky Way inferred from its circular velocity curve. MNRAS 528, 693–710 (2024). [45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021). Wyrzykowski, L. et al. The OGLE view of microlensing towards the Magellanic Clouds - IV. OGLE-III SMC data and final conclusions on MACHOs. MNRAS 416, 2949–2961 (2011). [18] Blaineau, T. et al. New limits from microlensing on Galactic black holes in the mass range 10 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT < M < 1000 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT. A&A 664, A106 (2022). [19] Udalski, A. The Optical Gravitational Lensing Experiment. Real Time Data Analysis Systems in the OGLE-III Survey. Acta Astron. 53, 291–305 (2003). [20] Mróz, P. et al. Microlensing optical depth and event rate toward the Large Magellanic Cloud based on 20 years of OGLE observations. submitted (2024). [21] Holtzman, J. A., Afonso, C. & Dolphin, A. The Local Group Stellar Populations Archive from the Hubble Space Telescope WFPC2. ApJS 166, 534–548 (2006). [22] Mróz, P. et al. No large population of unbound or wide-orbit Jupiter-mass planets. Nature 548, 183–186 (2017). [23] Cautun, M. et al. The milky way total mass profile as inferred from Gaia DR2. MNRAS 494, 4291–4313 (2020). [24] Han, C. & Gould, A. Stellar Contribution to the Galactic Bulge Microlensing Optical Depth. ApJ 592, 172–175 (2003). [25] Niikura, H. et al. Microlensing constraints on primordial black holes with Subaru/HSC Andromeda observations. Nature Astronomy 3, 524–534 (2019). [26] Sahu, K. C. Stars within the Large Magellanic Cloud as potential lenses for observed microlensing events. Nature 370, 275–276 (1994). [27] Erkal, D. et al. The total mass of the Large Magellanic Cloud from its perturbation on the Orphan stream. MNRAS 487, 2685–2700 (2019). [28] Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. A&A 678, A208 (2023). [29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. A distance to the Large Magellanic Cloud that is precise to one per cent. Nature 567, 200–203 (2019). [42] Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. An H I Aperture Synthesis Mosaic of the Large Magellanic Cloud. ApJ 503, 674–688 (1998). [44] Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. The dark matter profile of the Milky Way inferred from its circular velocity curve. MNRAS 528, 693–710 (2024). [45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021). Blaineau, T. et al. New limits from microlensing on Galactic black holes in the mass range 10 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT < M < 1000 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT. A&A 664, A106 (2022). [19] Udalski, A. The Optical Gravitational Lensing Experiment. Real Time Data Analysis Systems in the OGLE-III Survey. Acta Astron. 53, 291–305 (2003). [20] Mróz, P. et al. Microlensing optical depth and event rate toward the Large Magellanic Cloud based on 20 years of OGLE observations. submitted (2024). [21] Holtzman, J. A., Afonso, C. & Dolphin, A. The Local Group Stellar Populations Archive from the Hubble Space Telescope WFPC2. ApJS 166, 534–548 (2006). [22] Mróz, P. et al. No large population of unbound or wide-orbit Jupiter-mass planets. Nature 548, 183–186 (2017). [23] Cautun, M. et al. The milky way total mass profile as inferred from Gaia DR2. MNRAS 494, 4291–4313 (2020). [24] Han, C. & Gould, A. Stellar Contribution to the Galactic Bulge Microlensing Optical Depth. ApJ 592, 172–175 (2003). [25] Niikura, H. et al. Microlensing constraints on primordial black holes with Subaru/HSC Andromeda observations. Nature Astronomy 3, 524–534 (2019). [26] Sahu, K. C. Stars within the Large Magellanic Cloud as potential lenses for observed microlensing events. Nature 370, 275–276 (1994). [27] Erkal, D. et al. The total mass of the Large Magellanic Cloud from its perturbation on the Orphan stream. MNRAS 487, 2685–2700 (2019). [28] Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. A&A 678, A208 (2023). [29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. A distance to the Large Magellanic Cloud that is precise to one per cent. Nature 567, 200–203 (2019). [42] Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. An H I Aperture Synthesis Mosaic of the Large Magellanic Cloud. ApJ 503, 674–688 (1998). [44] Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. The dark matter profile of the Milky Way inferred from its circular velocity curve. MNRAS 528, 693–710 (2024). [45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021). Udalski, A. The Optical Gravitational Lensing Experiment. Real Time Data Analysis Systems in the OGLE-III Survey. Acta Astron. 53, 291–305 (2003). [20] Mróz, P. et al. Microlensing optical depth and event rate toward the Large Magellanic Cloud based on 20 years of OGLE observations. submitted (2024). [21] Holtzman, J. A., Afonso, C. & Dolphin, A. The Local Group Stellar Populations Archive from the Hubble Space Telescope WFPC2. ApJS 166, 534–548 (2006). [22] Mróz, P. et al. No large population of unbound or wide-orbit Jupiter-mass planets. Nature 548, 183–186 (2017). [23] Cautun, M. et al. The milky way total mass profile as inferred from Gaia DR2. MNRAS 494, 4291–4313 (2020). [24] Han, C. & Gould, A. Stellar Contribution to the Galactic Bulge Microlensing Optical Depth. ApJ 592, 172–175 (2003). [25] Niikura, H. et al. Microlensing constraints on primordial black holes with Subaru/HSC Andromeda observations. Nature Astronomy 3, 524–534 (2019). [26] Sahu, K. C. Stars within the Large Magellanic Cloud as potential lenses for observed microlensing events. Nature 370, 275–276 (1994). [27] Erkal, D. et al. The total mass of the Large Magellanic Cloud from its perturbation on the Orphan stream. MNRAS 487, 2685–2700 (2019). [28] Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. A&A 678, A208 (2023). [29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. A distance to the Large Magellanic Cloud that is precise to one per cent. Nature 567, 200–203 (2019). [42] Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. An H I Aperture Synthesis Mosaic of the Large Magellanic Cloud. ApJ 503, 674–688 (1998). [44] Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. The dark matter profile of the Milky Way inferred from its circular velocity curve. MNRAS 528, 693–710 (2024). [45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021). Mróz, P. et al. Microlensing optical depth and event rate toward the Large Magellanic Cloud based on 20 years of OGLE observations. submitted (2024). [21] Holtzman, J. A., Afonso, C. & Dolphin, A. The Local Group Stellar Populations Archive from the Hubble Space Telescope WFPC2. ApJS 166, 534–548 (2006). [22] Mróz, P. et al. No large population of unbound or wide-orbit Jupiter-mass planets. Nature 548, 183–186 (2017). [23] Cautun, M. et al. The milky way total mass profile as inferred from Gaia DR2. MNRAS 494, 4291–4313 (2020). [24] Han, C. & Gould, A. Stellar Contribution to the Galactic Bulge Microlensing Optical Depth. ApJ 592, 172–175 (2003). [25] Niikura, H. et al. Microlensing constraints on primordial black holes with Subaru/HSC Andromeda observations. Nature Astronomy 3, 524–534 (2019). [26] Sahu, K. C. Stars within the Large Magellanic Cloud as potential lenses for observed microlensing events. Nature 370, 275–276 (1994). [27] Erkal, D. et al. The total mass of the Large Magellanic Cloud from its perturbation on the Orphan stream. MNRAS 487, 2685–2700 (2019). [28] Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. A&A 678, A208 (2023). [29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. A distance to the Large Magellanic Cloud that is precise to one per cent. Nature 567, 200–203 (2019). [42] Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. An H I Aperture Synthesis Mosaic of the Large Magellanic Cloud. ApJ 503, 674–688 (1998). [44] Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. The dark matter profile of the Milky Way inferred from its circular velocity curve. MNRAS 528, 693–710 (2024). [45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021). Holtzman, J. A., Afonso, C. & Dolphin, A. The Local Group Stellar Populations Archive from the Hubble Space Telescope WFPC2. ApJS 166, 534–548 (2006). [22] Mróz, P. et al. No large population of unbound or wide-orbit Jupiter-mass planets. Nature 548, 183–186 (2017). [23] Cautun, M. et al. The milky way total mass profile as inferred from Gaia DR2. MNRAS 494, 4291–4313 (2020). [24] Han, C. & Gould, A. Stellar Contribution to the Galactic Bulge Microlensing Optical Depth. ApJ 592, 172–175 (2003). 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Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. 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J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. 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The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. 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MNRAS 487, 2685–2700 (2019). [28] Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. A&A 678, A208 (2023). [29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. A distance to the Large Magellanic Cloud that is precise to one per cent. Nature 567, 200–203 (2019). [42] Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. An H I Aperture Synthesis Mosaic of the Large Magellanic Cloud. ApJ 503, 674–688 (1998). [44] Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. The dark matter profile of the Milky Way inferred from its circular velocity curve. MNRAS 528, 693–710 (2024). [45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021). Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. A&A 678, A208 (2023). [29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. 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New limits from microlensing on Galactic black holes in the mass range 10 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT < M < 1000 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT. A&A 664, A106 (2022). [19] Udalski, A. The Optical Gravitational Lensing Experiment. Real Time Data Analysis Systems in the OGLE-III Survey. Acta Astron. 53, 291–305 (2003). [20] Mróz, P. et al. Microlensing optical depth and event rate toward the Large Magellanic Cloud based on 20 years of OGLE observations. submitted (2024). [21] Holtzman, J. A., Afonso, C. & Dolphin, A. The Local Group Stellar Populations Archive from the Hubble Space Telescope WFPC2. ApJS 166, 534–548 (2006). [22] Mróz, P. et al. No large population of unbound or wide-orbit Jupiter-mass planets. Nature 548, 183–186 (2017). [23] Cautun, M. et al. The milky way total mass profile as inferred from Gaia DR2. MNRAS 494, 4291–4313 (2020). [24] Han, C. & Gould, A. Stellar Contribution to the Galactic Bulge Microlensing Optical Depth. ApJ 592, 172–175 (2003). [25] Niikura, H. et al. Microlensing constraints on primordial black holes with Subaru/HSC Andromeda observations. Nature Astronomy 3, 524–534 (2019). [26] Sahu, K. C. Stars within the Large Magellanic Cloud as potential lenses for observed microlensing events. Nature 370, 275–276 (1994). [27] Erkal, D. et al. The total mass of the Large Magellanic Cloud from its perturbation on the Orphan stream. MNRAS 487, 2685–2700 (2019). [28] Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. A&A 678, A208 (2023). [29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. 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A&A 664, A106 (2022). [19] Udalski, A. The Optical Gravitational Lensing Experiment. Real Time Data Analysis Systems in the OGLE-III Survey. Acta Astron. 53, 291–305 (2003). [20] Mróz, P. et al. Microlensing optical depth and event rate toward the Large Magellanic Cloud based on 20 years of OGLE observations. submitted (2024). [21] Holtzman, J. A., Afonso, C. & Dolphin, A. The Local Group Stellar Populations Archive from the Hubble Space Telescope WFPC2. ApJS 166, 534–548 (2006). [22] Mróz, P. et al. No large population of unbound or wide-orbit Jupiter-mass planets. Nature 548, 183–186 (2017). [23] Cautun, M. et al. The milky way total mass profile as inferred from Gaia DR2. MNRAS 494, 4291–4313 (2020). [24] Han, C. & Gould, A. Stellar Contribution to the Galactic Bulge Microlensing Optical Depth. ApJ 592, 172–175 (2003). [25] Niikura, H. et al. Microlensing constraints on primordial black holes with Subaru/HSC Andromeda observations. Nature Astronomy 3, 524–534 (2019). [26] Sahu, K. C. Stars within the Large Magellanic Cloud as potential lenses for observed microlensing events. Nature 370, 275–276 (1994). [27] Erkal, D. et al. The total mass of the Large Magellanic Cloud from its perturbation on the Orphan stream. MNRAS 487, 2685–2700 (2019). [28] Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. A&A 678, A208 (2023). [29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. A distance to the Large Magellanic Cloud that is precise to one per cent. Nature 567, 200–203 (2019). [42] Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. An H I Aperture Synthesis Mosaic of the Large Magellanic Cloud. ApJ 503, 674–688 (1998). [44] Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. The dark matter profile of the Milky Way inferred from its circular velocity curve. MNRAS 528, 693–710 (2024). [45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021). Alcock, C. et al. The MACHO Project: Microlensing Results from 5.7 Years of Large Magellanic Cloud Observations. ApJ 542, 281–307 (2000). [16] Tisserand, P. et al. Limits on the Macho content of the Galactic Halo from the EROS-2 Survey of the Magellanic Clouds. A&A 469, 387–404 (2007). [17] Wyrzykowski, L. et al. The OGLE view of microlensing towards the Magellanic Clouds - IV. OGLE-III SMC data and final conclusions on MACHOs. MNRAS 416, 2949–2961 (2011). [18] Blaineau, T. et al. New limits from microlensing on Galactic black holes in the mass range 10 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT < M < 1000 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT. A&A 664, A106 (2022). [19] Udalski, A. The Optical Gravitational Lensing Experiment. Real Time Data Analysis Systems in the OGLE-III Survey. Acta Astron. 53, 291–305 (2003). [20] Mróz, P. et al. Microlensing optical depth and event rate toward the Large Magellanic Cloud based on 20 years of OGLE observations. submitted (2024). [21] Holtzman, J. A., Afonso, C. & Dolphin, A. The Local Group Stellar Populations Archive from the Hubble Space Telescope WFPC2. ApJS 166, 534–548 (2006). [22] Mróz, P. et al. No large population of unbound or wide-orbit Jupiter-mass planets. Nature 548, 183–186 (2017). [23] Cautun, M. et al. The milky way total mass profile as inferred from Gaia DR2. MNRAS 494, 4291–4313 (2020). [24] Han, C. & Gould, A. Stellar Contribution to the Galactic Bulge Microlensing Optical Depth. ApJ 592, 172–175 (2003). [25] Niikura, H. et al. Microlensing constraints on primordial black holes with Subaru/HSC Andromeda observations. Nature Astronomy 3, 524–534 (2019). [26] Sahu, K. C. Stars within the Large Magellanic Cloud as potential lenses for observed microlensing events. Nature 370, 275–276 (1994). [27] Erkal, D. et al. The total mass of the Large Magellanic Cloud from its perturbation on the Orphan stream. MNRAS 487, 2685–2700 (2019). [28] Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. A&A 678, A208 (2023). [29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. A distance to the Large Magellanic Cloud that is precise to one per cent. Nature 567, 200–203 (2019). [42] Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. An H I Aperture Synthesis Mosaic of the Large Magellanic Cloud. ApJ 503, 674–688 (1998). [44] Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. The dark matter profile of the Milky Way inferred from its circular velocity curve. MNRAS 528, 693–710 (2024). [45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021). Tisserand, P. et al. Limits on the Macho content of the Galactic Halo from the EROS-2 Survey of the Magellanic Clouds. A&A 469, 387–404 (2007). [17] Wyrzykowski, L. et al. The OGLE view of microlensing towards the Magellanic Clouds - IV. OGLE-III SMC data and final conclusions on MACHOs. MNRAS 416, 2949–2961 (2011). [18] Blaineau, T. et al. New limits from microlensing on Galactic black holes in the mass range 10 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT < M < 1000 M⊙direct-product{}_{{\odot}}start_FLOATSUBSCRIPT ⊙ end_FLOATSUBSCRIPT. A&A 664, A106 (2022). [19] Udalski, A. The Optical Gravitational Lensing Experiment. Real Time Data Analysis Systems in the OGLE-III Survey. Acta Astron. 53, 291–305 (2003). [20] Mróz, P. et al. Microlensing optical depth and event rate toward the Large Magellanic Cloud based on 20 years of OGLE observations. submitted (2024). [21] Holtzman, J. A., Afonso, C. & Dolphin, A. The Local Group Stellar Populations Archive from the Hubble Space Telescope WFPC2. ApJS 166, 534–548 (2006). [22] Mróz, P. et al. No large population of unbound or wide-orbit Jupiter-mass planets. Nature 548, 183–186 (2017). [23] Cautun, M. et al. The milky way total mass profile as inferred from Gaia DR2. MNRAS 494, 4291–4313 (2020). [24] Han, C. & Gould, A. Stellar Contribution to the Galactic Bulge Microlensing Optical Depth. ApJ 592, 172–175 (2003). [25] Niikura, H. et al. Microlensing constraints on primordial black holes with Subaru/HSC Andromeda observations. Nature Astronomy 3, 524–534 (2019). [26] Sahu, K. C. Stars within the Large Magellanic Cloud as potential lenses for observed microlensing events. Nature 370, 275–276 (1994). [27] Erkal, D. et al. The total mass of the Large Magellanic Cloud from its perturbation on the Orphan stream. MNRAS 487, 2685–2700 (2019). [28] Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. A&A 678, A208 (2023). [29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. A distance to the Large Magellanic Cloud that is precise to one per cent. Nature 567, 200–203 (2019). [42] Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. An H I Aperture Synthesis Mosaic of the Large Magellanic Cloud. ApJ 503, 674–688 (1998). [44] Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. The dark matter profile of the Milky Way inferred from its circular velocity curve. MNRAS 528, 693–710 (2024). [45] Gaia Collaboration et al. Gaia Data Release 2. 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Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. 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[39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. A distance to the Large Magellanic Cloud that is precise to one per cent. Nature 567, 200–203 (2019). [42] Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. An H I Aperture Synthesis Mosaic of the Large Magellanic Cloud. ApJ 503, 674–688 (1998). [44] Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. The dark matter profile of the Milky Way inferred from its circular velocity curve. MNRAS 528, 693–710 (2024). [45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021). Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. 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The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. 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The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. 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[37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. A distance to the Large Magellanic Cloud that is precise to one per cent. Nature 567, 200–203 (2019). [42] Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. An H I Aperture Synthesis Mosaic of the Large Magellanic Cloud. ApJ 503, 674–688 (1998). [44] Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. 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The milky way total mass profile as inferred from Gaia DR2. MNRAS 494, 4291–4313 (2020). [24] Han, C. & Gould, A. Stellar Contribution to the Galactic Bulge Microlensing Optical Depth. ApJ 592, 172–175 (2003). [25] Niikura, H. et al. Microlensing constraints on primordial black holes with Subaru/HSC Andromeda observations. Nature Astronomy 3, 524–534 (2019). [26] Sahu, K. C. Stars within the Large Magellanic Cloud as potential lenses for observed microlensing events. Nature 370, 275–276 (1994). [27] Erkal, D. et al. The total mass of the Large Magellanic Cloud from its perturbation on the Orphan stream. MNRAS 487, 2685–2700 (2019). [28] Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. A&A 678, A208 (2023). [29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. 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[45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021). Mróz, P. et al. Microlensing optical depth and event rate toward the Large Magellanic Cloud based on 20 years of OGLE observations. submitted (2024). [21] Holtzman, J. A., Afonso, C. & Dolphin, A. The Local Group Stellar Populations Archive from the Hubble Space Telescope WFPC2. ApJS 166, 534–548 (2006). [22] Mróz, P. et al. No large population of unbound or wide-orbit Jupiter-mass planets. Nature 548, 183–186 (2017). [23] Cautun, M. et al. The milky way total mass profile as inferred from Gaia DR2. MNRAS 494, 4291–4313 (2020). [24] Han, C. & Gould, A. Stellar Contribution to the Galactic Bulge Microlensing Optical Depth. ApJ 592, 172–175 (2003). [25] Niikura, H. et al. Microlensing constraints on primordial black holes with Subaru/HSC Andromeda observations. Nature Astronomy 3, 524–534 (2019). [26] Sahu, K. C. Stars within the Large Magellanic Cloud as potential lenses for observed microlensing events. Nature 370, 275–276 (1994). [27] Erkal, D. et al. The total mass of the Large Magellanic Cloud from its perturbation on the Orphan stream. MNRAS 487, 2685–2700 (2019). [28] Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. A&A 678, A208 (2023). [29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. A distance to the Large Magellanic Cloud that is precise to one per cent. Nature 567, 200–203 (2019). [42] Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. An H I Aperture Synthesis Mosaic of the Large Magellanic Cloud. ApJ 503, 674–688 (1998). [44] Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. The dark matter profile of the Milky Way inferred from its circular velocity curve. MNRAS 528, 693–710 (2024). [45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021). Holtzman, J. A., Afonso, C. & Dolphin, A. The Local Group Stellar Populations Archive from the Hubble Space Telescope WFPC2. ApJS 166, 534–548 (2006). [22] Mróz, P. et al. No large population of unbound or wide-orbit Jupiter-mass planets. Nature 548, 183–186 (2017). [23] Cautun, M. et al. The milky way total mass profile as inferred from Gaia DR2. MNRAS 494, 4291–4313 (2020). [24] Han, C. & Gould, A. Stellar Contribution to the Galactic Bulge Microlensing Optical Depth. ApJ 592, 172–175 (2003). [25] Niikura, H. et al. Microlensing constraints on primordial black holes with Subaru/HSC Andromeda observations. Nature Astronomy 3, 524–534 (2019). [26] Sahu, K. C. Stars within the Large Magellanic Cloud as potential lenses for observed microlensing events. Nature 370, 275–276 (1994). [27] Erkal, D. et al. The total mass of the Large Magellanic Cloud from its perturbation on the Orphan stream. MNRAS 487, 2685–2700 (2019). [28] Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. A&A 678, A208 (2023). [29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. A distance to the Large Magellanic Cloud that is precise to one per cent. Nature 567, 200–203 (2019). [42] Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. An H I Aperture Synthesis Mosaic of the Large Magellanic Cloud. ApJ 503, 674–688 (1998). [44] Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. The dark matter profile of the Milky Way inferred from its circular velocity curve. MNRAS 528, 693–710 (2024). [45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021). Mróz, P. et al. No large population of unbound or wide-orbit Jupiter-mass planets. Nature 548, 183–186 (2017). [23] Cautun, M. et al. The milky way total mass profile as inferred from Gaia DR2. MNRAS 494, 4291–4313 (2020). [24] Han, C. & Gould, A. Stellar Contribution to the Galactic Bulge Microlensing Optical Depth. ApJ 592, 172–175 (2003). [25] Niikura, H. et al. Microlensing constraints on primordial black holes with Subaru/HSC Andromeda observations. Nature Astronomy 3, 524–534 (2019). [26] Sahu, K. C. Stars within the Large Magellanic Cloud as potential lenses for observed microlensing events. Nature 370, 275–276 (1994). [27] Erkal, D. et al. The total mass of the Large Magellanic Cloud from its perturbation on the Orphan stream. MNRAS 487, 2685–2700 (2019). [28] Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. A&A 678, A208 (2023). [29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. A distance to the Large Magellanic Cloud that is precise to one per cent. Nature 567, 200–203 (2019). [42] Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. An H I Aperture Synthesis Mosaic of the Large Magellanic Cloud. ApJ 503, 674–688 (1998). [44] Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. The dark matter profile of the Milky Way inferred from its circular velocity curve. MNRAS 528, 693–710 (2024). [45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021). Cautun, M. et al. The milky way total mass profile as inferred from Gaia DR2. MNRAS 494, 4291–4313 (2020). [24] Han, C. & Gould, A. Stellar Contribution to the Galactic Bulge Microlensing Optical Depth. ApJ 592, 172–175 (2003). [25] Niikura, H. et al. Microlensing constraints on primordial black holes with Subaru/HSC Andromeda observations. Nature Astronomy 3, 524–534 (2019). [26] Sahu, K. C. Stars within the Large Magellanic Cloud as potential lenses for observed microlensing events. Nature 370, 275–276 (1994). [27] Erkal, D. et al. The total mass of the Large Magellanic Cloud from its perturbation on the Orphan stream. MNRAS 487, 2685–2700 (2019). [28] Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. A&A 678, A208 (2023). [29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. A distance to the Large Magellanic Cloud that is precise to one per cent. Nature 567, 200–203 (2019). [42] Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. An H I Aperture Synthesis Mosaic of the Large Magellanic Cloud. ApJ 503, 674–688 (1998). [44] Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. The dark matter profile of the Milky Way inferred from its circular velocity curve. MNRAS 528, 693–710 (2024). [45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021). Han, C. & Gould, A. Stellar Contribution to the Galactic Bulge Microlensing Optical Depth. ApJ 592, 172–175 (2003). [25] Niikura, H. et al. Microlensing constraints on primordial black holes with Subaru/HSC Andromeda observations. Nature Astronomy 3, 524–534 (2019). [26] Sahu, K. C. Stars within the Large Magellanic Cloud as potential lenses for observed microlensing events. Nature 370, 275–276 (1994). [27] Erkal, D. et al. The total mass of the Large Magellanic Cloud from its perturbation on the Orphan stream. MNRAS 487, 2685–2700 (2019). [28] Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. A&A 678, A208 (2023). [29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. A distance to the Large Magellanic Cloud that is precise to one per cent. Nature 567, 200–203 (2019). [42] Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. An H I Aperture Synthesis Mosaic of the Large Magellanic Cloud. ApJ 503, 674–688 (1998). [44] Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. The dark matter profile of the Milky Way inferred from its circular velocity curve. MNRAS 528, 693–710 (2024). [45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021). Niikura, H. et al. Microlensing constraints on primordial black holes with Subaru/HSC Andromeda observations. Nature Astronomy 3, 524–534 (2019). [26] Sahu, K. C. Stars within the Large Magellanic Cloud as potential lenses for observed microlensing events. Nature 370, 275–276 (1994). [27] Erkal, D. et al. The total mass of the Large Magellanic Cloud from its perturbation on the Orphan stream. MNRAS 487, 2685–2700 (2019). [28] Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. A&A 678, A208 (2023). [29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. A distance to the Large Magellanic Cloud that is precise to one per cent. Nature 567, 200–203 (2019). [42] Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. An H I Aperture Synthesis Mosaic of the Large Magellanic Cloud. ApJ 503, 674–688 (1998). [44] Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. The dark matter profile of the Milky Way inferred from its circular velocity curve. MNRAS 528, 693–710 (2024). [45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021). Sahu, K. C. Stars within the Large Magellanic Cloud as potential lenses for observed microlensing events. Nature 370, 275–276 (1994). [27] Erkal, D. et al. The total mass of the Large Magellanic Cloud from its perturbation on the Orphan stream. MNRAS 487, 2685–2700 (2019). [28] Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. A&A 678, A208 (2023). [29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. A distance to the Large Magellanic Cloud that is precise to one per cent. Nature 567, 200–203 (2019). [42] Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. 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[37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. A distance to the Large Magellanic Cloud that is precise to one per cent. Nature 567, 200–203 (2019). [42] Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. An H I Aperture Synthesis Mosaic of the Large Magellanic Cloud. ApJ 503, 674–688 (1998). [44] Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. The dark matter profile of the Milky Way inferred from its circular velocity curve. MNRAS 528, 693–710 (2024). [45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021). Udalski, A. The Optical Gravitational Lensing Experiment. Real Time Data Analysis Systems in the OGLE-III Survey. Acta Astron. 53, 291–305 (2003). [20] Mróz, P. et al. Microlensing optical depth and event rate toward the Large Magellanic Cloud based on 20 years of OGLE observations. submitted (2024). [21] Holtzman, J. A., Afonso, C. & Dolphin, A. The Local Group Stellar Populations Archive from the Hubble Space Telescope WFPC2. ApJS 166, 534–548 (2006). [22] Mróz, P. et al. No large population of unbound or wide-orbit Jupiter-mass planets. Nature 548, 183–186 (2017). [23] Cautun, M. et al. The milky way total mass profile as inferred from Gaia DR2. MNRAS 494, 4291–4313 (2020). [24] Han, C. & Gould, A. Stellar Contribution to the Galactic Bulge Microlensing Optical Depth. ApJ 592, 172–175 (2003). [25] Niikura, H. et al. Microlensing constraints on primordial black holes with Subaru/HSC Andromeda observations. Nature Astronomy 3, 524–534 (2019). [26] Sahu, K. C. Stars within the Large Magellanic Cloud as potential lenses for observed microlensing events. Nature 370, 275–276 (1994). [27] Erkal, D. et al. The total mass of the Large Magellanic Cloud from its perturbation on the Orphan stream. MNRAS 487, 2685–2700 (2019). [28] Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. A&A 678, A208 (2023). [29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. A distance to the Large Magellanic Cloud that is precise to one per cent. Nature 567, 200–203 (2019). [42] Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. An H I Aperture Synthesis Mosaic of the Large Magellanic Cloud. ApJ 503, 674–688 (1998). [44] Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. The dark matter profile of the Milky Way inferred from its circular velocity curve. MNRAS 528, 693–710 (2024). [45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021). Mróz, P. et al. Microlensing optical depth and event rate toward the Large Magellanic Cloud based on 20 years of OGLE observations. submitted (2024). [21] Holtzman, J. A., Afonso, C. & Dolphin, A. The Local Group Stellar Populations Archive from the Hubble Space Telescope WFPC2. ApJS 166, 534–548 (2006). [22] Mróz, P. et al. No large population of unbound or wide-orbit Jupiter-mass planets. Nature 548, 183–186 (2017). [23] Cautun, M. et al. The milky way total mass profile as inferred from Gaia DR2. MNRAS 494, 4291–4313 (2020). [24] Han, C. & Gould, A. Stellar Contribution to the Galactic Bulge Microlensing Optical Depth. ApJ 592, 172–175 (2003). [25] Niikura, H. et al. Microlensing constraints on primordial black holes with Subaru/HSC Andromeda observations. Nature Astronomy 3, 524–534 (2019). [26] Sahu, K. C. Stars within the Large Magellanic Cloud as potential lenses for observed microlensing events. Nature 370, 275–276 (1994). [27] Erkal, D. et al. The total mass of the Large Magellanic Cloud from its perturbation on the Orphan stream. MNRAS 487, 2685–2700 (2019). [28] Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. A&A 678, A208 (2023). [29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. A distance to the Large Magellanic Cloud that is precise to one per cent. Nature 567, 200–203 (2019). [42] Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. An H I Aperture Synthesis Mosaic of the Large Magellanic Cloud. ApJ 503, 674–688 (1998). [44] Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. The dark matter profile of the Milky Way inferred from its circular velocity curve. MNRAS 528, 693–710 (2024). [45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021). Holtzman, J. A., Afonso, C. & Dolphin, A. The Local Group Stellar Populations Archive from the Hubble Space Telescope WFPC2. ApJS 166, 534–548 (2006). [22] Mróz, P. et al. No large population of unbound or wide-orbit Jupiter-mass planets. Nature 548, 183–186 (2017). [23] Cautun, M. et al. The milky way total mass profile as inferred from Gaia DR2. MNRAS 494, 4291–4313 (2020). [24] Han, C. & Gould, A. Stellar Contribution to the Galactic Bulge Microlensing Optical Depth. ApJ 592, 172–175 (2003). [25] Niikura, H. et al. Microlensing constraints on primordial black holes with Subaru/HSC Andromeda observations. Nature Astronomy 3, 524–534 (2019). [26] Sahu, K. C. Stars within the Large Magellanic Cloud as potential lenses for observed microlensing events. Nature 370, 275–276 (1994). [27] Erkal, D. et al. The total mass of the Large Magellanic Cloud from its perturbation on the Orphan stream. MNRAS 487, 2685–2700 (2019). [28] Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. A&A 678, A208 (2023). [29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. A distance to the Large Magellanic Cloud that is precise to one per cent. Nature 567, 200–203 (2019). [42] Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. An H I Aperture Synthesis Mosaic of the Large Magellanic Cloud. ApJ 503, 674–688 (1998). [44] Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. The dark matter profile of the Milky Way inferred from its circular velocity curve. MNRAS 528, 693–710 (2024). [45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021). Mróz, P. et al. No large population of unbound or wide-orbit Jupiter-mass planets. Nature 548, 183–186 (2017). [23] Cautun, M. et al. The milky way total mass profile as inferred from Gaia DR2. MNRAS 494, 4291–4313 (2020). [24] Han, C. & Gould, A. Stellar Contribution to the Galactic Bulge Microlensing Optical Depth. ApJ 592, 172–175 (2003). [25] Niikura, H. et al. Microlensing constraints on primordial black holes with Subaru/HSC Andromeda observations. Nature Astronomy 3, 524–534 (2019). [26] Sahu, K. C. Stars within the Large Magellanic Cloud as potential lenses for observed microlensing events. Nature 370, 275–276 (1994). [27] Erkal, D. et al. The total mass of the Large Magellanic Cloud from its perturbation on the Orphan stream. MNRAS 487, 2685–2700 (2019). [28] Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. A&A 678, A208 (2023). [29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. A distance to the Large Magellanic Cloud that is precise to one per cent. Nature 567, 200–203 (2019). [42] Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. An H I Aperture Synthesis Mosaic of the Large Magellanic Cloud. ApJ 503, 674–688 (1998). [44] Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. The dark matter profile of the Milky Way inferred from its circular velocity curve. MNRAS 528, 693–710 (2024). [45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021). Cautun, M. et al. The milky way total mass profile as inferred from Gaia DR2. MNRAS 494, 4291–4313 (2020). [24] Han, C. & Gould, A. Stellar Contribution to the Galactic Bulge Microlensing Optical Depth. ApJ 592, 172–175 (2003). [25] Niikura, H. et al. Microlensing constraints on primordial black holes with Subaru/HSC Andromeda observations. Nature Astronomy 3, 524–534 (2019). [26] Sahu, K. C. Stars within the Large Magellanic Cloud as potential lenses for observed microlensing events. Nature 370, 275–276 (1994). [27] Erkal, D. et al. The total mass of the Large Magellanic Cloud from its perturbation on the Orphan stream. MNRAS 487, 2685–2700 (2019). [28] Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. A&A 678, A208 (2023). [29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. A distance to the Large Magellanic Cloud that is precise to one per cent. Nature 567, 200–203 (2019). [42] Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. An H I Aperture Synthesis Mosaic of the Large Magellanic Cloud. ApJ 503, 674–688 (1998). [44] Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. The dark matter profile of the Milky Way inferred from its circular velocity curve. MNRAS 528, 693–710 (2024). [45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021). Han, C. & Gould, A. Stellar Contribution to the Galactic Bulge Microlensing Optical Depth. ApJ 592, 172–175 (2003). [25] Niikura, H. et al. Microlensing constraints on primordial black holes with Subaru/HSC Andromeda observations. Nature Astronomy 3, 524–534 (2019). [26] Sahu, K. C. Stars within the Large Magellanic Cloud as potential lenses for observed microlensing events. Nature 370, 275–276 (1994). [27] Erkal, D. et al. The total mass of the Large Magellanic Cloud from its perturbation on the Orphan stream. MNRAS 487, 2685–2700 (2019). [28] Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. 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[27] Erkal, D. et al. The total mass of the Large Magellanic Cloud from its perturbation on the Orphan stream. MNRAS 487, 2685–2700 (2019). [28] Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. A&A 678, A208 (2023). [29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. A distance to the Large Magellanic Cloud that is precise to one per cent. Nature 567, 200–203 (2019). [42] Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. An H I Aperture Synthesis Mosaic of the Large Magellanic Cloud. ApJ 503, 674–688 (1998). [44] Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. The dark matter profile of the Milky Way inferred from its circular velocity curve. MNRAS 528, 693–710 (2024). [45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021). Udalski, A. The Optical Gravitational Lensing Experiment. Real Time Data Analysis Systems in the OGLE-III Survey. Acta Astron. 53, 291–305 (2003). [20] Mróz, P. et al. 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The total mass of the Large Magellanic Cloud from its perturbation on the Orphan stream. MNRAS 487, 2685–2700 (2019). [28] Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. A&A 678, A208 (2023). [29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. 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The Local Group Stellar Populations Archive from the Hubble Space Telescope WFPC2. ApJS 166, 534–548 (2006). [22] Mróz, P. et al. No large population of unbound or wide-orbit Jupiter-mass planets. Nature 548, 183–186 (2017). [23] Cautun, M. et al. The milky way total mass profile as inferred from Gaia DR2. MNRAS 494, 4291–4313 (2020). [24] Han, C. & Gould, A. Stellar Contribution to the Galactic Bulge Microlensing Optical Depth. ApJ 592, 172–175 (2003). [25] Niikura, H. et al. Microlensing constraints on primordial black holes with Subaru/HSC Andromeda observations. Nature Astronomy 3, 524–534 (2019). [26] Sahu, K. C. Stars within the Large Magellanic Cloud as potential lenses for observed microlensing events. Nature 370, 275–276 (1994). [27] Erkal, D. et al. The total mass of the Large Magellanic Cloud from its perturbation on the Orphan stream. MNRAS 487, 2685–2700 (2019). [28] Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. A&A 678, A208 (2023). [29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. A distance to the Large Magellanic Cloud that is precise to one per cent. Nature 567, 200–203 (2019). [42] Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. An H I Aperture Synthesis Mosaic of the Large Magellanic Cloud. ApJ 503, 674–688 (1998). [44] Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. The dark matter profile of the Milky Way inferred from its circular velocity curve. MNRAS 528, 693–710 (2024). [45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021). Holtzman, J. A., Afonso, C. & Dolphin, A. The Local Group Stellar Populations Archive from the Hubble Space Telescope WFPC2. ApJS 166, 534–548 (2006). [22] Mróz, P. et al. No large population of unbound or wide-orbit Jupiter-mass planets. Nature 548, 183–186 (2017). [23] Cautun, M. et al. The milky way total mass profile as inferred from Gaia DR2. MNRAS 494, 4291–4313 (2020). [24] Han, C. & Gould, A. Stellar Contribution to the Galactic Bulge Microlensing Optical Depth. ApJ 592, 172–175 (2003). [25] Niikura, H. et al. Microlensing constraints on primordial black holes with Subaru/HSC Andromeda observations. Nature Astronomy 3, 524–534 (2019). [26] Sahu, K. C. Stars within the Large Magellanic Cloud as potential lenses for observed microlensing events. Nature 370, 275–276 (1994). [27] Erkal, D. et al. The total mass of the Large Magellanic Cloud from its perturbation on the Orphan stream. MNRAS 487, 2685–2700 (2019). [28] Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. A&A 678, A208 (2023). [29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. A distance to the Large Magellanic Cloud that is precise to one per cent. Nature 567, 200–203 (2019). [42] Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. An H I Aperture Synthesis Mosaic of the Large Magellanic Cloud. ApJ 503, 674–688 (1998). [44] Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. The dark matter profile of the Milky Way inferred from its circular velocity curve. MNRAS 528, 693–710 (2024). [45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. 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Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. A distance to the Large Magellanic Cloud that is precise to one per cent. Nature 567, 200–203 (2019). [42] Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. An H I Aperture Synthesis Mosaic of the Large Magellanic Cloud. ApJ 503, 674–688 (1998). [44] Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. The dark matter profile of the Milky Way inferred from its circular velocity curve. MNRAS 528, 693–710 (2024). [45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021). Cautun, M. et al. The milky way total mass profile as inferred from Gaia DR2. MNRAS 494, 4291–4313 (2020). [24] Han, C. & Gould, A. Stellar Contribution to the Galactic Bulge Microlensing Optical Depth. ApJ 592, 172–175 (2003). [25] Niikura, H. et al. Microlensing constraints on primordial black holes with Subaru/HSC Andromeda observations. Nature Astronomy 3, 524–534 (2019). [26] Sahu, K. C. Stars within the Large Magellanic Cloud as potential lenses for observed microlensing events. Nature 370, 275–276 (1994). [27] Erkal, D. et al. The total mass of the Large Magellanic Cloud from its perturbation on the Orphan stream. MNRAS 487, 2685–2700 (2019). [28] Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. A&A 678, A208 (2023). [29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. 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The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. 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[25] Niikura, H. et al. Microlensing constraints on primordial black holes with Subaru/HSC Andromeda observations. Nature Astronomy 3, 524–534 (2019). [26] Sahu, K. C. Stars within the Large Magellanic Cloud as potential lenses for observed microlensing events. Nature 370, 275–276 (1994). [27] Erkal, D. et al. The total mass of the Large Magellanic Cloud from its perturbation on the Orphan stream. MNRAS 487, 2685–2700 (2019). [28] Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. A&A 678, A208 (2023). [29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. 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[27] Erkal, D. et al. The total mass of the Large Magellanic Cloud from its perturbation on the Orphan stream. MNRAS 487, 2685–2700 (2019). [28] Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. A&A 678, A208 (2023). [29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. 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[23] Cautun, M. et al. The milky way total mass profile as inferred from Gaia DR2. MNRAS 494, 4291–4313 (2020). [24] Han, C. & Gould, A. Stellar Contribution to the Galactic Bulge Microlensing Optical Depth. ApJ 592, 172–175 (2003). [25] Niikura, H. et al. Microlensing constraints on primordial black holes with Subaru/HSC Andromeda observations. Nature Astronomy 3, 524–534 (2019). [26] Sahu, K. C. Stars within the Large Magellanic Cloud as potential lenses for observed microlensing events. Nature 370, 275–276 (1994). [27] Erkal, D. et al. The total mass of the Large Magellanic Cloud from its perturbation on the Orphan stream. MNRAS 487, 2685–2700 (2019). [28] Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. A&A 678, A208 (2023). [29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. 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MNRAS 487, 2685–2700 (2019). [28] Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. A&A 678, A208 (2023). [29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. A distance to the Large Magellanic Cloud that is precise to one per cent. Nature 567, 200–203 (2019). [42] Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. An H I Aperture Synthesis Mosaic of the Large Magellanic Cloud. ApJ 503, 674–688 (1998). [44] Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. The dark matter profile of the Milky Way inferred from its circular velocity curve. MNRAS 528, 693–710 (2024). [45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021). Cautun, M. et al. The milky way total mass profile as inferred from Gaia DR2. MNRAS 494, 4291–4313 (2020). [24] Han, C. & Gould, A. Stellar Contribution to the Galactic Bulge Microlensing Optical Depth. ApJ 592, 172–175 (2003). [25] Niikura, H. et al. Microlensing constraints on primordial black holes with Subaru/HSC Andromeda observations. Nature Astronomy 3, 524–534 (2019). [26] Sahu, K. C. Stars within the Large Magellanic Cloud as potential lenses for observed microlensing events. Nature 370, 275–276 (1994). [27] Erkal, D. et al. The total mass of the Large Magellanic Cloud from its perturbation on the Orphan stream. MNRAS 487, 2685–2700 (2019). [28] Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. A&A 678, A208 (2023). [29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. A distance to the Large Magellanic Cloud that is precise to one per cent. Nature 567, 200–203 (2019). [42] Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. An H I Aperture Synthesis Mosaic of the Large Magellanic Cloud. ApJ 503, 674–688 (1998). [44] Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. The dark matter profile of the Milky Way inferred from its circular velocity curve. MNRAS 528, 693–710 (2024). [45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021). Han, C. & Gould, A. Stellar Contribution to the Galactic Bulge Microlensing Optical Depth. ApJ 592, 172–175 (2003). [25] Niikura, H. et al. Microlensing constraints on primordial black holes with Subaru/HSC Andromeda observations. Nature Astronomy 3, 524–534 (2019). [26] Sahu, K. C. Stars within the Large Magellanic Cloud as potential lenses for observed microlensing events. Nature 370, 275–276 (1994). [27] Erkal, D. et al. The total mass of the Large Magellanic Cloud from its perturbation on the Orphan stream. MNRAS 487, 2685–2700 (2019). [28] Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. A&A 678, A208 (2023). [29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. 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The dark matter profile of the Milky Way inferred from its circular velocity curve. MNRAS 528, 693–710 (2024). [45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021). Mróz, P. et al. Microlensing optical depth and event rate toward the Large Magellanic Cloud based on 20 years of OGLE observations. submitted (2024). [21] Holtzman, J. A., Afonso, C. & Dolphin, A. The Local Group Stellar Populations Archive from the Hubble Space Telescope WFPC2. ApJS 166, 534–548 (2006). [22] Mróz, P. et al. No large population of unbound or wide-orbit Jupiter-mass planets. Nature 548, 183–186 (2017). [23] Cautun, M. et al. The milky way total mass profile as inferred from Gaia DR2. MNRAS 494, 4291–4313 (2020). [24] Han, C. & Gould, A. Stellar Contribution to the Galactic Bulge Microlensing Optical Depth. ApJ 592, 172–175 (2003). [25] Niikura, H. et al. Microlensing constraints on primordial black holes with Subaru/HSC Andromeda observations. Nature Astronomy 3, 524–534 (2019). [26] Sahu, K. C. Stars within the Large Magellanic Cloud as potential lenses for observed microlensing events. Nature 370, 275–276 (1994). [27] Erkal, D. et al. The total mass of the Large Magellanic Cloud from its perturbation on the Orphan stream. MNRAS 487, 2685–2700 (2019). [28] Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. A&A 678, A208 (2023). [29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. A distance to the Large Magellanic Cloud that is precise to one per cent. Nature 567, 200–203 (2019). [42] Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. An H I Aperture Synthesis Mosaic of the Large Magellanic Cloud. ApJ 503, 674–688 (1998). [44] Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. The dark matter profile of the Milky Way inferred from its circular velocity curve. MNRAS 528, 693–710 (2024). [45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021). Holtzman, J. A., Afonso, C. & Dolphin, A. The Local Group Stellar Populations Archive from the Hubble Space Telescope WFPC2. ApJS 166, 534–548 (2006). [22] Mróz, P. et al. No large population of unbound or wide-orbit Jupiter-mass planets. Nature 548, 183–186 (2017). [23] Cautun, M. et al. The milky way total mass profile as inferred from Gaia DR2. MNRAS 494, 4291–4313 (2020). [24] Han, C. & Gould, A. Stellar Contribution to the Galactic Bulge Microlensing Optical Depth. ApJ 592, 172–175 (2003). [25] Niikura, H. et al. Microlensing constraints on primordial black holes with Subaru/HSC Andromeda observations. Nature Astronomy 3, 524–534 (2019). [26] Sahu, K. C. Stars within the Large Magellanic Cloud as potential lenses for observed microlensing events. Nature 370, 275–276 (1994). [27] Erkal, D. et al. The total mass of the Large Magellanic Cloud from its perturbation on the Orphan stream. MNRAS 487, 2685–2700 (2019). [28] Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. A&A 678, A208 (2023). [29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. A distance to the Large Magellanic Cloud that is precise to one per cent. Nature 567, 200–203 (2019). [42] Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. An H I Aperture Synthesis Mosaic of the Large Magellanic Cloud. ApJ 503, 674–688 (1998). [44] Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. The dark matter profile of the Milky Way inferred from its circular velocity curve. MNRAS 528, 693–710 (2024). [45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021). Mróz, P. et al. No large population of unbound or wide-orbit Jupiter-mass planets. Nature 548, 183–186 (2017). [23] Cautun, M. et al. The milky way total mass profile as inferred from Gaia DR2. MNRAS 494, 4291–4313 (2020). [24] Han, C. & Gould, A. Stellar Contribution to the Galactic Bulge Microlensing Optical Depth. ApJ 592, 172–175 (2003). [25] Niikura, H. et al. Microlensing constraints on primordial black holes with Subaru/HSC Andromeda observations. Nature Astronomy 3, 524–534 (2019). [26] Sahu, K. C. Stars within the Large Magellanic Cloud as potential lenses for observed microlensing events. Nature 370, 275–276 (1994). [27] Erkal, D. et al. The total mass of the Large Magellanic Cloud from its perturbation on the Orphan stream. MNRAS 487, 2685–2700 (2019). [28] Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. A&A 678, A208 (2023). [29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. A distance to the Large Magellanic Cloud that is precise to one per cent. Nature 567, 200–203 (2019). [42] Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. An H I Aperture Synthesis Mosaic of the Large Magellanic Cloud. ApJ 503, 674–688 (1998). [44] Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. The dark matter profile of the Milky Way inferred from its circular velocity curve. MNRAS 528, 693–710 (2024). [45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021). Cautun, M. et al. The milky way total mass profile as inferred from Gaia DR2. MNRAS 494, 4291–4313 (2020). [24] Han, C. & Gould, A. Stellar Contribution to the Galactic Bulge Microlensing Optical Depth. ApJ 592, 172–175 (2003). [25] Niikura, H. et al. Microlensing constraints on primordial black holes with Subaru/HSC Andromeda observations. Nature Astronomy 3, 524–534 (2019). [26] Sahu, K. C. Stars within the Large Magellanic Cloud as potential lenses for observed microlensing events. Nature 370, 275–276 (1994). [27] Erkal, D. et al. The total mass of the Large Magellanic Cloud from its perturbation on the Orphan stream. MNRAS 487, 2685–2700 (2019). [28] Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. A&A 678, A208 (2023). [29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. A distance to the Large Magellanic Cloud that is precise to one per cent. Nature 567, 200–203 (2019). [42] Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. An H I Aperture Synthesis Mosaic of the Large Magellanic Cloud. ApJ 503, 674–688 (1998). [44] Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. The dark matter profile of the Milky Way inferred from its circular velocity curve. MNRAS 528, 693–710 (2024). [45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021). Han, C. & Gould, A. Stellar Contribution to the Galactic Bulge Microlensing Optical Depth. ApJ 592, 172–175 (2003). [25] Niikura, H. et al. Microlensing constraints on primordial black holes with Subaru/HSC Andromeda observations. Nature Astronomy 3, 524–534 (2019). [26] Sahu, K. C. Stars within the Large Magellanic Cloud as potential lenses for observed microlensing events. Nature 370, 275–276 (1994). [27] Erkal, D. et al. The total mass of the Large Magellanic Cloud from its perturbation on the Orphan stream. MNRAS 487, 2685–2700 (2019). [28] Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. A&A 678, A208 (2023). [29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. A distance to the Large Magellanic Cloud that is precise to one per cent. Nature 567, 200–203 (2019). [42] Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. An H I Aperture Synthesis Mosaic of the Large Magellanic Cloud. ApJ 503, 674–688 (1998). [44] Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. The dark matter profile of the Milky Way inferred from its circular velocity curve. MNRAS 528, 693–710 (2024). [45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021). Niikura, H. et al. Microlensing constraints on primordial black holes with Subaru/HSC Andromeda observations. Nature Astronomy 3, 524–534 (2019). [26] Sahu, K. C. Stars within the Large Magellanic Cloud as potential lenses for observed microlensing events. Nature 370, 275–276 (1994). [27] Erkal, D. et al. The total mass of the Large Magellanic Cloud from its perturbation on the Orphan stream. MNRAS 487, 2685–2700 (2019). [28] Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. A&A 678, A208 (2023). [29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. A distance to the Large Magellanic Cloud that is precise to one per cent. Nature 567, 200–203 (2019). [42] Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. An H I Aperture Synthesis Mosaic of the Large Magellanic Cloud. ApJ 503, 674–688 (1998). [44] Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. The dark matter profile of the Milky Way inferred from its circular velocity curve. MNRAS 528, 693–710 (2024). [45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021). Sahu, K. C. Stars within the Large Magellanic Cloud as potential lenses for observed microlensing events. Nature 370, 275–276 (1994). [27] Erkal, D. et al. The total mass of the Large Magellanic Cloud from its perturbation on the Orphan stream. MNRAS 487, 2685–2700 (2019). [28] Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. A&A 678, A208 (2023). [29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). 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Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. 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[23] Cautun, M. et al. The milky way total mass profile as inferred from Gaia DR2. MNRAS 494, 4291–4313 (2020). [24] Han, C. & Gould, A. Stellar Contribution to the Galactic Bulge Microlensing Optical Depth. ApJ 592, 172–175 (2003). [25] Niikura, H. et al. Microlensing constraints on primordial black holes with Subaru/HSC Andromeda observations. Nature Astronomy 3, 524–534 (2019). [26] Sahu, K. C. Stars within the Large Magellanic Cloud as potential lenses for observed microlensing events. Nature 370, 275–276 (1994). [27] Erkal, D. et al. The total mass of the Large Magellanic Cloud from its perturbation on the Orphan stream. MNRAS 487, 2685–2700 (2019). [28] Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. A&A 678, A208 (2023). [29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. 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[45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021). Mróz, P. et al. No large population of unbound or wide-orbit Jupiter-mass planets. Nature 548, 183–186 (2017). [23] Cautun, M. et al. The milky way total mass profile as inferred from Gaia DR2. MNRAS 494, 4291–4313 (2020). [24] Han, C. & Gould, A. Stellar Contribution to the Galactic Bulge Microlensing Optical Depth. ApJ 592, 172–175 (2003). [25] Niikura, H. et al. Microlensing constraints on primordial black holes with Subaru/HSC Andromeda observations. Nature Astronomy 3, 524–534 (2019). [26] Sahu, K. C. Stars within the Large Magellanic Cloud as potential lenses for observed microlensing events. Nature 370, 275–276 (1994). [27] Erkal, D. et al. The total mass of the Large Magellanic Cloud from its perturbation on the Orphan stream. MNRAS 487, 2685–2700 (2019). [28] Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. A&A 678, A208 (2023). [29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. A distance to the Large Magellanic Cloud that is precise to one per cent. Nature 567, 200–203 (2019). [42] Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. An H I Aperture Synthesis Mosaic of the Large Magellanic Cloud. ApJ 503, 674–688 (1998). [44] Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. The dark matter profile of the Milky Way inferred from its circular velocity curve. MNRAS 528, 693–710 (2024). [45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021). Cautun, M. et al. The milky way total mass profile as inferred from Gaia DR2. MNRAS 494, 4291–4313 (2020). [24] Han, C. & Gould, A. Stellar Contribution to the Galactic Bulge Microlensing Optical Depth. ApJ 592, 172–175 (2003). [25] Niikura, H. et al. Microlensing constraints on primordial black holes with Subaru/HSC Andromeda observations. Nature Astronomy 3, 524–534 (2019). [26] Sahu, K. C. Stars within the Large Magellanic Cloud as potential lenses for observed microlensing events. Nature 370, 275–276 (1994). [27] Erkal, D. et al. The total mass of the Large Magellanic Cloud from its perturbation on the Orphan stream. MNRAS 487, 2685–2700 (2019). [28] Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. A&A 678, A208 (2023). [29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. A distance to the Large Magellanic Cloud that is precise to one per cent. Nature 567, 200–203 (2019). [42] Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. An H I Aperture Synthesis Mosaic of the Large Magellanic Cloud. ApJ 503, 674–688 (1998). [44] Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. The dark matter profile of the Milky Way inferred from its circular velocity curve. MNRAS 528, 693–710 (2024). [45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021). Han, C. & Gould, A. Stellar Contribution to the Galactic Bulge Microlensing Optical Depth. ApJ 592, 172–175 (2003). [25] Niikura, H. et al. Microlensing constraints on primordial black holes with Subaru/HSC Andromeda observations. Nature Astronomy 3, 524–534 (2019). [26] Sahu, K. C. Stars within the Large Magellanic Cloud as potential lenses for observed microlensing events. Nature 370, 275–276 (1994). [27] Erkal, D. et al. The total mass of the Large Magellanic Cloud from its perturbation on the Orphan stream. MNRAS 487, 2685–2700 (2019). [28] Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. A&A 678, A208 (2023). [29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. A distance to the Large Magellanic Cloud that is precise to one per cent. Nature 567, 200–203 (2019). [42] Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. An H I Aperture Synthesis Mosaic of the Large Magellanic Cloud. ApJ 503, 674–688 (1998). [44] Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. The dark matter profile of the Milky Way inferred from its circular velocity curve. MNRAS 528, 693–710 (2024). [45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021). Niikura, H. et al. Microlensing constraints on primordial black holes with Subaru/HSC Andromeda observations. Nature Astronomy 3, 524–534 (2019). [26] Sahu, K. C. Stars within the Large Magellanic Cloud as potential lenses for observed microlensing events. Nature 370, 275–276 (1994). [27] Erkal, D. et al. The total mass of the Large Magellanic Cloud from its perturbation on the Orphan stream. MNRAS 487, 2685–2700 (2019). [28] Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. A&A 678, A208 (2023). [29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. A distance to the Large Magellanic Cloud that is precise to one per cent. Nature 567, 200–203 (2019). [42] Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. An H I Aperture Synthesis Mosaic of the Large Magellanic Cloud. ApJ 503, 674–688 (1998). [44] Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. The dark matter profile of the Milky Way inferred from its circular velocity curve. MNRAS 528, 693–710 (2024). [45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021). Sahu, K. C. Stars within the Large Magellanic Cloud as potential lenses for observed microlensing events. Nature 370, 275–276 (1994). [27] Erkal, D. et al. The total mass of the Large Magellanic Cloud from its perturbation on the Orphan stream. MNRAS 487, 2685–2700 (2019). [28] Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. A&A 678, A208 (2023). [29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. A distance to the Large Magellanic Cloud that is precise to one per cent. Nature 567, 200–203 (2019). [42] Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. An H I Aperture Synthesis Mosaic of the Large Magellanic Cloud. ApJ 503, 674–688 (1998). [44] Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. The dark matter profile of the Milky Way inferred from its circular velocity curve. MNRAS 528, 693–710 (2024). [45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021). Erkal, D. et al. The total mass of the Large Magellanic Cloud from its perturbation on the Orphan stream. MNRAS 487, 2685–2700 (2019). [28] Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. A&A 678, A208 (2023). [29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. 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[23] Cautun, M. et al. The milky way total mass profile as inferred from Gaia DR2. MNRAS 494, 4291–4313 (2020). [24] Han, C. & Gould, A. Stellar Contribution to the Galactic Bulge Microlensing Optical Depth. ApJ 592, 172–175 (2003). [25] Niikura, H. et al. Microlensing constraints on primordial black holes with Subaru/HSC Andromeda observations. Nature Astronomy 3, 524–534 (2019). [26] Sahu, K. C. Stars within the Large Magellanic Cloud as potential lenses for observed microlensing events. Nature 370, 275–276 (1994). [27] Erkal, D. et al. The total mass of the Large Magellanic Cloud from its perturbation on the Orphan stream. MNRAS 487, 2685–2700 (2019). [28] Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. A&A 678, A208 (2023). [29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. 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[45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021). Mróz, P. et al. No large population of unbound or wide-orbit Jupiter-mass planets. Nature 548, 183–186 (2017). [23] Cautun, M. et al. The milky way total mass profile as inferred from Gaia DR2. MNRAS 494, 4291–4313 (2020). [24] Han, C. & Gould, A. Stellar Contribution to the Galactic Bulge Microlensing Optical Depth. ApJ 592, 172–175 (2003). [25] Niikura, H. et al. Microlensing constraints on primordial black holes with Subaru/HSC Andromeda observations. Nature Astronomy 3, 524–534 (2019). [26] Sahu, K. C. Stars within the Large Magellanic Cloud as potential lenses for observed microlensing events. Nature 370, 275–276 (1994). [27] Erkal, D. et al. The total mass of the Large Magellanic Cloud from its perturbation on the Orphan stream. 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Nature Astronomy 3, 524–534 (2019). [26] Sahu, K. C. Stars within the Large Magellanic Cloud as potential lenses for observed microlensing events. Nature 370, 275–276 (1994). [27] Erkal, D. et al. The total mass of the Large Magellanic Cloud from its perturbation on the Orphan stream. MNRAS 487, 2685–2700 (2019). [28] Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. A&A 678, A208 (2023). [29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. 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Stellar Contribution to the Galactic Bulge Microlensing Optical Depth. ApJ 592, 172–175 (2003). [25] Niikura, H. et al. Microlensing constraints on primordial black holes with Subaru/HSC Andromeda observations. Nature Astronomy 3, 524–534 (2019). [26] Sahu, K. C. Stars within the Large Magellanic Cloud as potential lenses for observed microlensing events. Nature 370, 275–276 (1994). [27] Erkal, D. et al. The total mass of the Large Magellanic Cloud from its perturbation on the Orphan stream. MNRAS 487, 2685–2700 (2019). [28] Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. A&A 678, A208 (2023). [29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. 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On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. A distance to the Large Magellanic Cloud that is precise to one per cent. Nature 567, 200–203 (2019). [42] Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. An H I Aperture Synthesis Mosaic of the Large Magellanic Cloud. ApJ 503, 674–688 (1998). [44] Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. The dark matter profile of the Milky Way inferred from its circular velocity curve. MNRAS 528, 693–710 (2024). [45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021). Niikura, H. et al. Microlensing constraints on primordial black holes with Subaru/HSC Andromeda observations. Nature Astronomy 3, 524–534 (2019). [26] Sahu, K. C. Stars within the Large Magellanic Cloud as potential lenses for observed microlensing events. Nature 370, 275–276 (1994). [27] Erkal, D. et al. The total mass of the Large Magellanic Cloud from its perturbation on the Orphan stream. MNRAS 487, 2685–2700 (2019). [28] Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. A&A 678, A208 (2023). [29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. 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[24] Han, C. & Gould, A. Stellar Contribution to the Galactic Bulge Microlensing Optical Depth. ApJ 592, 172–175 (2003). [25] Niikura, H. et al. Microlensing constraints on primordial black holes with Subaru/HSC Andromeda observations. Nature Astronomy 3, 524–534 (2019). [26] Sahu, K. C. Stars within the Large Magellanic Cloud as potential lenses for observed microlensing events. Nature 370, 275–276 (1994). [27] Erkal, D. et al. The total mass of the Large Magellanic Cloud from its perturbation on the Orphan stream. MNRAS 487, 2685–2700 (2019). [28] Jiao, Y. et al. Detection of the Keplerian decline in the Milky Way rotation curve. A&A 678, A208 (2023). [29] Clanton, C. & Gaudi, B. S. Synthesizing Exoplanet Demographics from Radial Velocity and Microlensing Surveys. I. Methodology. ApJ 791, 90 (2014). [30] Eilers, A.-C., Hogg, D. W., Rix, H.-W. & Ness, M. K. The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. 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MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. A distance to the Large Magellanic Cloud that is precise to one per cent. Nature 567, 200–203 (2019). [42] Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. An H I Aperture Synthesis Mosaic of the Large Magellanic Cloud. ApJ 503, 674–688 (1998). [44] Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. The dark matter profile of the Milky Way inferred from its circular velocity curve. MNRAS 528, 693–710 (2024). [45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021). Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. A distance to the Large Magellanic Cloud that is precise to one per cent. Nature 567, 200–203 (2019). [42] Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. An H I Aperture Synthesis Mosaic of the Large Magellanic Cloud. ApJ 503, 674–688 (1998). [44] Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. The dark matter profile of the Milky Way inferred from its circular velocity curve. MNRAS 528, 693–710 (2024). [45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021). Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. A distance to the Large Magellanic Cloud that is precise to one per cent. Nature 567, 200–203 (2019). [42] Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. An H I Aperture Synthesis Mosaic of the Large Magellanic Cloud. ApJ 503, 674–688 (1998). [44] Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. The dark matter profile of the Milky Way inferred from its circular velocity curve. MNRAS 528, 693–710 (2024). [45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021). Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. A distance to the Large Magellanic Cloud that is precise to one per cent. Nature 567, 200–203 (2019). [42] Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. An H I Aperture Synthesis Mosaic of the Large Magellanic Cloud. ApJ 503, 674–688 (1998). [44] Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. The dark matter profile of the Milky Way inferred from its circular velocity curve. MNRAS 528, 693–710 (2024). [45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021). Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. A distance to the Large Magellanic Cloud that is precise to one per cent. Nature 567, 200–203 (2019). [42] Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. An H I Aperture Synthesis Mosaic of the Large Magellanic Cloud. ApJ 503, 674–688 (1998). [44] Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. The dark matter profile of the Milky Way inferred from its circular velocity curve. MNRAS 528, 693–710 (2024). [45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021). Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. 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The dark matter profile of the Milky Way inferred from its circular velocity curve. MNRAS 528, 693–710 (2024). [45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021). Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. A distance to the Large Magellanic Cloud that is precise to one per cent. Nature 567, 200–203 (2019). [42] Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. An H I Aperture Synthesis Mosaic of the Large Magellanic Cloud. ApJ 503, 674–688 (1998). [44] Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. The dark matter profile of the Milky Way inferred from its circular velocity curve. MNRAS 528, 693–710 (2024). [45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021). van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. A distance to the Large Magellanic Cloud that is precise to one per cent. Nature 567, 200–203 (2019). [42] Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. An H I Aperture Synthesis Mosaic of the Large Magellanic Cloud. ApJ 503, 674–688 (1998). [44] Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. The dark matter profile of the Milky Way inferred from its circular velocity curve. MNRAS 528, 693–710 (2024). [45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021). Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. A distance to the Large Magellanic Cloud that is precise to one per cent. Nature 567, 200–203 (2019). [42] Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. An H I Aperture Synthesis Mosaic of the Large Magellanic Cloud. ApJ 503, 674–688 (1998). [44] Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. The dark matter profile of the Milky Way inferred from its circular velocity curve. MNRAS 528, 693–710 (2024). [45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021). Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. A distance to the Large Magellanic Cloud that is precise to one per cent. Nature 567, 200–203 (2019). [42] Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. An H I Aperture Synthesis Mosaic of the Large Magellanic Cloud. ApJ 503, 674–688 (1998). [44] Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. The dark matter profile of the Milky Way inferred from its circular velocity curve. MNRAS 528, 693–710 (2024). [45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021). van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. A distance to the Large Magellanic Cloud that is precise to one per cent. Nature 567, 200–203 (2019). [42] Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. An H I Aperture Synthesis Mosaic of the Large Magellanic Cloud. ApJ 503, 674–688 (1998). [44] Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. The dark matter profile of the Milky Way inferred from its circular velocity curve. MNRAS 528, 693–710 (2024). [45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021). Pietrzyński, G. et al. A distance to the Large Magellanic Cloud that is precise to one per cent. Nature 567, 200–203 (2019). [42] Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. An H I Aperture Synthesis Mosaic of the Large Magellanic Cloud. ApJ 503, 674–688 (1998). [44] Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. The dark matter profile of the Milky Way inferred from its circular velocity curve. MNRAS 528, 693–710 (2024). [45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021). Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. An H I Aperture Synthesis Mosaic of the Large Magellanic Cloud. ApJ 503, 674–688 (1998). [44] Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. The dark matter profile of the Milky Way inferred from its circular velocity curve. MNRAS 528, 693–710 (2024). [45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021). Kim, S. et al. An H I Aperture Synthesis Mosaic of the Large Magellanic Cloud. ApJ 503, 674–688 (1998). [44] Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. The dark matter profile of the Milky Way inferred from its circular velocity curve. MNRAS 528, 693–710 (2024). [45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021). Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. The dark matter profile of the Milky Way inferred from its circular velocity curve. MNRAS 528, 693–710 (2024). [45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021). Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021). Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021).
- The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. ApJ 871, 120 (2019). [31] Schaye, J. et al. The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS 446, 521–554 (2015). [32] Fattahi, A. et al. The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection. MNRAS 457, 844–856 (2016). [33] Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. A distance to the Large Magellanic Cloud that is precise to one per cent. Nature 567, 200–203 (2019). [42] Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. An H I Aperture Synthesis Mosaic of the Large Magellanic Cloud. ApJ 503, 674–688 (1998). [44] Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. 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Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. A distance to the Large Magellanic Cloud that is precise to one per cent. Nature 567, 200–203 (2019). [42] Foreman-Mackey, D., Hogg, D. 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[42] Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. An H I Aperture Synthesis Mosaic of the Large Magellanic Cloud. ApJ 503, 674–688 (1998). [44] Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. The dark matter profile of the Milky Way inferred from its circular velocity curve. MNRAS 528, 693–710 (2024). [45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021). Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. MNRAS 467, 179–207 (2017). [34] Griest, K. et al. Gravitational microlensing as a method of detecting disk dark matter and faint disk stars. ApJ 372, L79–L82 (1991). [35] Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. 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The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. A distance to the Large Magellanic Cloud that is precise to one per cent. Nature 567, 200–203 (2019). [42] Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. An H I Aperture Synthesis Mosaic of the Large Magellanic Cloud. ApJ 503, 674–688 (1998). [44] Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. The dark matter profile of the Milky Way inferred from its circular velocity curve. MNRAS 528, 693–710 (2024). [45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021). Varma, V. et al. Evidence of Large Recoil Velocity from a Black Hole Merger Signal. Phys. Rev. Lett. 128, 191102 (2022). [36] Koposov, S. E. et al. Piercing the Milky Way: an all-sky view of the Orphan Stream. MNRAS 485, 4726–4742 (2019). [37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. 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[37] van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. A distance to the Large Magellanic Cloud that is precise to one per cent. Nature 567, 200–203 (2019). [42] Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. An H I Aperture Synthesis Mosaic of the Large Magellanic Cloud. ApJ 503, 674–688 (1998). [44] Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. The dark matter profile of the Milky Way inferred from its circular velocity curve. MNRAS 528, 693–710 (2024). [45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021). van der Marel, R. P. & Kallivayalil, N. Third-epoch Magellanic Cloud Proper Motions. II. The Large Magellanic Cloud Rotation Field in Three Dimensions. ApJ 781, 121 (2014). [38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. A distance to the Large Magellanic Cloud that is precise to one per cent. Nature 567, 200–203 (2019). [42] Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. An H I Aperture Synthesis Mosaic of the Large Magellanic Cloud. ApJ 503, 674–688 (1998). [44] Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. The dark matter profile of the Milky Way inferred from its circular velocity curve. MNRAS 528, 693–710 (2024). [45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021). Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. 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[40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. A distance to the Large Magellanic Cloud that is precise to one per cent. Nature 567, 200–203 (2019). [42] Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. An H I Aperture Synthesis Mosaic of the Large Magellanic Cloud. ApJ 503, 674–688 (1998). [44] Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. The dark matter profile of the Milky Way inferred from its circular velocity curve. MNRAS 528, 693–710 (2024). [45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021). van der Marel, R. P., Alves, D. 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A distance to the Large Magellanic Cloud that is precise to one per cent. Nature 567, 200–203 (2019). [42] Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. An H I Aperture Synthesis Mosaic of the Large Magellanic Cloud. ApJ 503, 674–688 (1998). [44] Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. The dark matter profile of the Milky Way inferred from its circular velocity curve. MNRAS 528, 693–710 (2024). [45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021). Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. An H I Aperture Synthesis Mosaic of the Large Magellanic Cloud. ApJ 503, 674–688 (1998). [44] Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. The dark matter profile of the Milky Way inferred from its circular velocity curve. MNRAS 528, 693–710 (2024). [45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021). Kim, S. et al. An H I Aperture Synthesis Mosaic of the Large Magellanic Cloud. ApJ 503, 674–688 (1998). [44] Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. The dark matter profile of the Milky Way inferred from its circular velocity curve. MNRAS 528, 693–710 (2024). [45] Gaia Collaboration et al. Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way. A&A 616, A12 (2018). [46] Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021). Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. The dark matter profile of the Milky Way inferred from its circular velocity curve. 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[38] Kroupa, P. On the variation of the initial mass function. MNRAS 322, 231–246 (2001). [39] Gyuk, G., Dalal, N. & Griest, K. Self-lensing Models of the Large Magellanic Cloud. ApJ 535, 90–103 (2000). [40] van der Marel, R. P., Alves, D. R., Hardy, E. & Suntzeff, N. B. New Understanding of Large Magellanic Cloud Structure, Dynamics, and Orbit from Carbon Star Kinematics. AJ 124, 2639–2663 (2002). [41] Pietrzyński, G. et al. A distance to the Large Magellanic Cloud that is precise to one per cent. Nature 567, 200–203 (2019). [42] Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. PASP 125, 306 (2013). [43] Kim, S. et al. An H I Aperture Synthesis Mosaic of the Large Magellanic Cloud. ApJ 503, 674–688 (1998). [44] Ou, X., Eilers, A.-C., Necib, L. & Frebel, A. The dark matter profile of the Milky Way inferred from its circular velocity curve. MNRAS 528, 693–710 (2024). [45] Gaia Collaboration et al. Gaia Data Release 2. 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- Lindegren, L. et al. Gaia Early Data Release 3. The astrometric solution. A&A 649, A2 (2021).
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