1811.10604
Astrophyiscs with radioactive isotopes
Diehl
1811.10607
Formation of ultra-diffuse galaxies in the field and in galaxy groups
Jian, Dekel, et al
Study UDGs in zoom in cosmo sims, seeing the origins of UDGs in the field versus galaxy groups. Find that while field UDGs arise from dwarfs in a characteristic mass range by multiple episodes of SN feedback, group UDGs may also form by tidal puffing up and they become quiescent by ram-pressure stripping. The field and group UDGs share similar properties, independent of distance from the group centre. Their DM haloes have ordinary spin parameters and centrally dominant DM cores. Their stellar component tend to have a prolate shape with a Sersic index n~1 but no significant rotation. Ram pressure removes the gas from the group UDGs when they are at pericentre, quenching SF in them and making them redder. This generates a color/SFR gradient with distance from the center, as observed in clusters. Find that ~20% of the field UDGs that fall into a massive halo survive as satellite UDGs. In addition, normal field dwarfs on highly eccentric orbits can become UDGs near pericentre due to tidal puffing up, contributing about half of the group-UDG pupation. Interpret the findings using simple toy models, showing that gas stripping is mostly due to ram pressure than tides. Estimate that the energy deposited by tides in the bound component of a satellite over one orbit can cause significant puffing up provided that the orbit is sufficiently eccentric.
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