📝 SummarXiv

Abstract

Stellar substructures within tidal debris preserve information about their progenitor galaxies' properties, offering insights into hierarchical mass assembly. We examine a compact stellar system (CSS) around the nearby spiral galaxy NGC 7531, including the shell-like tidal debris. Our goals are to determine the nature of the CSS, reconstruct the accretion history, and understand how the large, diffuse shell-like structure formed. We present photometric measurements of the shell-like debris and CSS using DESI Legacy Imaging Survey (LS) data. We obtained Keck/LRIS spectroscopic data for the CSS to confirm its association with NGC 7531 and to derive its star formation history (SFH). Deep ($\sim$27.9 mag/arcsec$^{2}$) amateur telescope images enabled complete characterization of the tidal debris structure. We confirm the CSS is associated with NGC 7531. We rename it NGC 7531-UCD1, since its stellar mass ($3.7_{-0.7}^{+1.0}\times 10^6$ $\mathrm{M}_\odot$), half-light radius ($R_{h} = 0.13 \pm 0.05$ arcsec) and SFH place it as an ultra-compact dwarf galaxy (UCD). NGC 7531-UCD1 was likely a nuclear star cluster (NSC) that was tidally stripped into a UCD- this is further supported by the presence of tidal tails. We quantify the shell-like debris' mass as $M_\star\sim 3$--$11\times 10^8 M_\odot$, implying a merger mass ratio of ~300:1 to 10:1. Our amateur telescope images confirm new pieces of debris, previously unclear in the DESI LS images. N-body simulations reproduce the tidal features, requiring a near radial orbit of the progenitor with two pericentric passages. The first passage coincides with the measured star formation enhancement ~1 Gyr ago. Our findings agree with predictions about the NSC to UCD formation pathway via tidal stripping, and further confirm the presence of these objects outside of our Milky Way.