The Andromeda galaxy's most important merger about 2 billion years ago as M32's likely progenitor (1807.08819v1)

Abstract: Although the proximity of the Andromeda galaxy (M31) offers an opportunity to understand how mergers affect galaxies, uncertainty remains about M31's most important mergers. Previous studies focused individually on the giant stellar stream or the impact of M32 on M31's disk, thereby suggesting many substantial satellite interactions. Yet models of M31's disk heating and the similarity between the stellar populations of different tidal substructures in M31's outskirts both suggested a single large merger. M31's stellar halo (its outer low-surface-brightness regions) is built up from the tidal debris of satellites and provides information about its important mergers. Here we use cosmological models of galaxy formation to show that M31's massive and metal-rich stellar halo, containing intermediate-age stars, dramatically narrows the range of allowed interactions, requiring a single dominant merger with a large galaxy (with stellar mass about 2.5 x 10^10 solar masses, the third largest member of the Local Group) about 2 Gyr ago. This single event explains many observations that were previously considered separately: M31's compact and metal-rich satellite M32 is likely to be the stripped core of the disrupted galaxy, its rotating inner stellar halo contains most of the merger debris, and the giant stellar stream is likely to have been thrown out during the merger. This interaction may explain M31's global burst of star formation about 2 Gyr ago in which approximately a fifth of its stars were formed. Moreover, M31's disk and bulge were already in place, suggesting that mergers of this magnitude need not dramatically affect galaxy structure.

• The paper demonstrates that a singular major merger around 2 billion years ago drove Andromeda's evolution, challenging earlier multiple merger models.
• It employs detailed cosmological simulations, including the Illustris hydrodynamical models, to isolate M31 analogues and confirm the merger with a metal-rich, high star-formation progenitor.
• Results highlight that M32 is likely the stripped core of this massive progenitor, reshaping our understanding of galactic structure resilience post-merger.

A Study of Andromeda Galaxy’s Prominent Merger Event and M32’s Progenitors

The paper by Richard D’Souza and Eric F. Bell explores the past of the Andromeda Galaxy (M31), proposing a significant merger event that occurred approximately 2 billion years ago. Extensive cosmological modeling and observational data are used to argue that M31's prominent merger involved the accretion of a large, metal-rich galaxy, asserting that M32, M31's compact satellite galaxy, stands as the likely remnant core of this disrupted massive progenitor.

The authors provide robust evidence suggesting a solitary dominant merger exerted substantial influence on M31's stellar halo and overall galactic structure. The paper decisively pivots from earlier hypotheses centered on numerous significant minor mergers, instead asserting a singular massive interaction as the most viable historical scenario.

Key Insights and Methodologies

Distinct cosmological simulations, including the Illustris hydrodynamical simulations, form the backbone of the authors’ analysis. Through these models, they isolate a subset of M31 analogues, which reveals a narrowed accretion history consistent with a major merger event. The simulations predict that galaxies similar to M31, with their acquired stellar characteristics, likely result from the merger of a metal-rich progenitor with substantial mass, characterized by active star formation and defined metallicity gradients.

Indeed, the paper postulates that M32's compact nature, along with its metallicity and stellar formation history, aligns well with it being the stripped core of this larger progenitor, termed M32p. Critical findings, such as M31's global burst of star formation around 2 billion years ago and the origin of its rotating inner stellar halo, emphasize the role of one significant progenitor.

Implications

The implications of these findings are broad, both for our understanding of M31's evolution and galactic formation theories at large. On a practical level, this scenario implies that large-scale mergers do not necessitate dramatic restructuring of galaxy disks, as evidenced by M31's extant disk configuration prior to the merger. This finding may influence existing models regarding galaxy morphology's resilience to major but singular disruptions. Furthermore, the correlation of M32 with the giant stellar stream and the metal-rich debris emphasizes the significant impact singular events can have on halo morphology and composition.

Future Speculations

The paper’s conclusions open avenues for verifying analogous situations in other galaxies, expanding the role of cosmological simulations in reconstructing elusive galactic histories. Moreover, the findings may prompt reevaluation of similar cases where compact elliptical galaxies like M32 are remnants of larger progenitors. This research arguably underscores the necessity for high-resolution models that can precisely map past galactic interactions and distill comprehensive evolutionary timelines.

Conclusion

D'Souza and Bell present a compelling narrative that characterizes M31's historical development, foregrounded by a significant singular merger event that shaped its current structural and compositional attributes. This inquiry not only elucidates Andromeda’s past but enriches broader discourses on the impacts of major cosmic mergers, refining our understanding of galactic evolution and structural dynamics.