Signatures of the M31-M32 Galactic Collision

TL;DR

This paper presents a detailed self-consistent model of the recent collision between the Andromeda galaxy (M31) and its dwarf companion M32, explaining their observed structures and dynamics without requiring a rare orbit.

Contribution

It provides the first comprehensive model of the M31-M32 interaction that matches observed positions, velocities, and morphologies, challenging previous assumptions about their collision orbit.

Findings

Andromeda's ring-like structure can form without a head-on collision.

M32's stars are not significantly tidally stripped during the interaction.

M32 is likely closer to the Milky Way than previously thought.

Abstract

The unusual morphologies of the Andromeda spiral galaxy (M31) and its dwarf companion M32 have been characterized observationally in great detail. The two galaxies' apparent proximity suggests that Andromeda's prominent star-forming ring as well as M32's compact elliptical structure may result from a recent collision. Here we present the first self-consistent model of the M31-M32 interaction that simultaneously reproduces observed positions, velocities, and morphologies for both galaxies. Andromeda's spiral structure is resolved in unprecedented detail, showing that a rare head-on orbit is not necessary to match Andromeda's ring-like morphology. The passage of M32 through Andromeda's disk perturbs the disk velocity structure. We find tidal stripping of M32's stars to be inefficient during the interaction, suggesting that some cEs are intrinsically compact. Additionally, the orbital solution implies that M32 is currently closer to the Milky Way than models have typically assumed, a prediction that may be testable with upcoming observations.