http://arxiv.org/abs/1908.05684
We study the origins of 122 ultra-diffuse galaxies (UDGs) in the RomulusC zoom-in cosmological simulation of a galaxy cluster (M${200} = 1.15 \times 10^{14}$ M${\odot}$), one of the only such simulations capable of resolving the evolution and structure of dwarf galaxies (M${\star} < 10^9$ M${\odot}$). We find broad agreement with observed cluster UDGs and predict that they are not separate from the overall cluster dwarf population. UDGs in cluster environments form primarily due to the quenching of star formation from ram pressure stripping and the subsequent passive evolution of their stellar population which results in very low surface brightness dwarf galaxies. We predict that there is little difference between UDGs and non-UDGs in terms of their dark matter halo masses and spins, their $z = 0$ colors, nor their evolution over time. UDGs are typically larger dwarf galaxies well before in-fall into the cluster and have had their star formation quenched for longer, typically due to entering the cluster earlier. We find that in most respects cluster UDG and non-UDGs alike are similar to isolated dwarf galaxies, although they are typically larger in size. This is due, in part, to the fact that cluster dwarf galaxies grow from higher angular momentum gas compared to isolated dwarf galaxies.
M. Tremmel, A. Wright, A. Brooks, et. al.
Mon, 19 Aug 19
32/46
Comments: 23 Pages, 18 Figures, Submitted to MNRAS. Comments are welcome!
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