Origin and evolution of ultra-diffuse galaxies in different environments

Abstract

We study the formation of ultra-diffuse galaxies (UDGs) using the cosmological hydrodynamical simulation TNG50 of the Illustris-TNG suite. We define UDGs as dwarf galaxies in the stellar mass range $7.5\le \log ({\mathrm{M}}_{\star }/{\mathrm{M}}_{\odot })\le 9$ that are in the $5\%$ most extended tail of the simulated mass-size relation. This results in a sample of UDGs with half-mass radii ${\mathrm{r}}_{\mathrm{h}\star }\gtrsim 2\mathrm{kpc}$ and surface brightness between $24.5$ and $28\mathrm{mag}\mathrm{arcse}{\mathrm{c}}^{-2}$, similar to definitions of UDGs in observations. The large cosmological volume in TNG50 allows for a comparison of UDGs properties in different environments, from the field to galaxy clusters with virial mass ${\mathrm{M}}_{200}\sim 2\times 10^{14}{\mathrm{M}}_{\odot }$. All UDGs in our sample have dwarf-mass haloes (${\mathrm{M}}_{200}\sim 10^{11}{\mathrm{M}}_{\odot }$) and show the same environmental trends as normal dwarfs: field UDGs are star-forming and blue while satellite UDGs are typically quiescent and red. The TNG50 simulation predicts UDGs that populate preferentially higher spin haloes and more massive haloes at fixed ${\mathrm{M}}_{\star }$ compared to non-UDG dwarfs. This applies also to most satellite UDGs, which are actually ``born" UDGs in the field and infall into groups and clusters without significant changes to their size. We find, however, a small subset of satellite UDGs ($\lesssim 10\%$) with present-day stellar size a factor $\ge 1.5$ larger than at infall, confirming that tidal effects, particularly in the lower mass dwarfs, are also a viable formation mechanism for some of these dwarfs, although subdominant in this simulation.

arXiv comment17 pages, 14 figures, accepted to MNRAS

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