PS J2305+3714: A Gravitationally Lensed Quasar

• The paper demonstrates a precise 52.2 ± 2.5 day time-delay measurement using modified dispersion minimization and spline methods.
• It employs high-precision, multi-year optical photometry, spectroscopy, and astrometry to determine accurate redshifts and flux ratios.
• The work advances time-delay cosmography with reliable mass models and minimal microlensing, supporting robust H0 estimations.

The gravitationally lensed quasar system PS J2305+3714 is a doubly imaged quasar lens established as a robust cosmographic probe through extensive multi-year optical photometric monitoring, follow-up spectroscopy, high-precision astrometry, and mass modeling. It is characterized by its clean time-domain variability, minimal microlensing, and well-constrained mass and redshift properties, qualifying it as an exemplary system for future time-delay cosmography and Hubble constant ($H_0$) determinations.

1. Observational Properties and Photometric Monitoring

PS J2305+3714 was observed over seven seasons (2018–2024) using the 1.5 m Maidanak Telescope in the Bessel R band. The campaign utilized SNUCAM and Andor XL detectors, each with $4096 \times 4096$ or $4096 \times 4108$ pixels and gain/read noise parameters tailored for high-precision photometry. Observational sampling consisted of either $5 \times 300$ s or $8 \times 180$ s nightly exposures, totaling 1472 frames. Median seeing was $1.29'' \pm 0.13''$.

PSF photometry was performed with IMFITFITS, modeling two lensed quasar images (A, B) plus the lensing galaxy using positions fixed by HST astrometry. After discarding 3% of frames for quality control, nightly-averaged light curves spanning 258 nights achieved photometric precisions of $\sigma_A = 0.005$ mag and $\sigma_B = 0.009$ mag. The amplitude of any secular microlensing variability in A or B did not exceed 10 mmag on the 7-year baseline (Burkhonov et al., 3 Jan 2026).

2. Time-Delay Measurement Methods and Results

The time delay between images A and B was measured using a modified $D^2_4$ dispersion minimization algorithm with Gaussian weighting ($\delta$ ranging from 5 to 25 d). Across optimal $4096 \times 4096$0 values (10–20 d), peak delays were consistently in the 52–53 d range with intrinsic scatter $4096 \times 4096$10.4 d. Bootstrap uncertainty estimation, incorporating 1000 realizations and epoch-dependent photometric errors, yielded $4096 \times 4096$2 days for $4096 \times 4096$3 d. Inclusion of linear microlensing produced $4096 \times 4096$4 days. For a conservative compilation, the final delay is reported as:

$4096 \times 4096$5

with image A leading B. Spline-based delay estimation (Millon et al. 2020) corroborates the central value, albeit with larger formal uncertainties ($4096 \times 4096$64 d) (Burkhonov et al., 3 Jan 2026).

3. Spectroscopic Redshift Determination

Analysis of WHT/ISIS long-slit spectroscopy (R300B blue, R158 red; $4096 \times 4096$7 s exposures) enabled spatial deblending of A, B, and the lensing galaxy using Moffat profile fitting. Quasar redshift was determined by modeling the Mg II $4096 \times 4096$8 region with a power-law continuum plus Fe II template and Gaussian line, yielding:

$4096 \times 4096$9

The lens galaxy redshift was extracted from absorption features (Ca II H&K, G-band, H$4096 \times 4108$0), producing the first direct measurement:

$4096 \times 4108$1

This spectroscopic precision underpins the subsequent cosmological analyses (Burkhonov et al., 3 Jan 2026).

4. Flux Ratio Analysis and Microlensing Constraints

Using the Mg II fit, the observed brightness ratios were:

• B/A in Mg II: $4096 \times 4108$2
• B/A in adjacent continuum (2800 Å): $4096 \times 4108$3

The Mg II emission originates from the broad-line region and is negligibly affected by microlensing, while the continuum emanates from a compact accretion disk. The minimal difference in ratios ($4096 \times 4108$4) between these domains indicates negligible differential microlensing, fully consistent with the weak microlensing signal observed in the light curves (amplitude $4096 \times 4108$5 mmag over 7 years) (Burkhonov et al., 3 Jan 2026).

5. Astrometric Characterization and Mass Modeling

High-precision astrometry from HST/ACS/WFC F814W imaging (2 × 337 s, 2023) determined the positions and magnitudes of system components with sub-milliarcsecond uncertainties. Relative positions (arcsec, A at 0,0) are:

• A: (0.000, 0.000), 17.38 mag
• B: (1.460, 1.645), 18.54 mag
• G (galaxy): (1.183, 0.853), 18.13 mag

The lens light profile parameters were $4096 \times 4108$6 (effective radius), $4096 \times 4108$7 (axis ratio), and $4096 \times 4108$8 (position angle).

Mass models were constructed using gravlens/lensmodel software with cosmological parameters ($4096 \times 4108$9 km s⁻¹ Mpc⁻¹, $5 \times 300$0, $5 \times 300$1):

• Singular Isothermal Sphere plus external shear (SIS+$5 \times 300$2): $5 \times 300$3, $5 \times 300$4, predicted $5 \times 300$5 d
• Power-law Ellipsoid (SIE, $5 \times 300$6): $5 \times 300$7, $5 \times 300$8, $5 \times 300$9, $8 \times 180$0, predicted $8 \times 180$1 d

These models predict time delays in close agreement with the measured value. For reference, rescaling theoretical delay predictions (Shajib et al. 2021) from ($8 \times 180$2, $8 \times 180$3) to ($8 \times 180$4, $8 \times 180$5) yields 55.2 d, also consistent with the empirical result (Burkhonov et al., 3 Jan 2026).

6. Role in Time-Delay Cosmography

PS J2305+3714 fulfills criteria required for its application in time-delay cosmography. The composite data show:

• Precise delay: $8 \times 180$6 d (A leads B)
• Accurate redshifts: $8 \times 180$7, $8 \times 180$8
• High-fidelity astrometry from HST
• Flux ratios from the broad-line region with minimal microlensing
• Simple, well-tested mass models yielding self-consistent delays

These attributes ensure reliable modeling of the lens geometry and cosmological distances within a concordance $8 \times 180$9CDM framework. PS J2305+3714 is thus prioritized for future determinations of $1.29'' \pm 0.13''$0 and as a calibrator system once additional measurements—specifically stellar kinematics of the lens and line-of-sight convergence—are acquired. A plausible implication is the system’s utility for controlling lens model systematics and constraining cosmological parameters at the percent level (Burkhonov et al., 3 Jan 2026).

7. Comparison and Context

Unlike quadruple-image lenses such as PS1 J0147+4630 (Berghea et al., 2017), which exhibit pronounced flux-ratio anomalies due to strong microlensing and millilensing, PS J2305+3714 is notable for its very low microlensing amplitude and straightforward isothermal mass profile modeling. This difference underscores its suitability for cosmographic applications, as complicated substructure effects are largely absent. The results from PS J2305+3714 broaden the portfolio of time-delay lenses with well-controlled systematics, complementing the more complex quad systems that probe small-scale structure and dark matter subhalos.

In summary, PS J2305+3714 embodies the defining characteristics of a benchmark “double” lens: minimal microlensing, high-fidelity time-delay, precise spectroscopic and astrometric parameters, and mass models that predict delays consistent with direct observations—solidifying its position as a key resource for gravitational lens cosmography and Hubble constant investigations (Burkhonov et al., 3 Jan 2026).