| Title | The Formation History of Subhalos and the Evolution of Satellite Galaxies |
| Authors | Shi, Jingjing Wang, Huiyuan Mo, Houjun Vogelsberger, Mark Ho, Luis C. Du, Min Nelson, Dylan Pillepich, Annalisa Hernquist, Lars |
| Affiliation | Peking Univ, Kavli Inst Astron & Astrophys, Beijing 100871, Peoples R China Univ Tokyo, UTIAS, Kavli IPMU WPI, Kashiwa, Chiba 2778583, Japan Univ Sci & Technol China, Dept Astron, Key Lab Res Galaxies & Cosmol, Hefei 230026, Anhui, Peoples R China Univ Sci & Technol China, Sch Astron & Space Sci, Hefei 230026, Peoples R China Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA Tsinghua Univ, Astron Dept, Beijing 10084, Peoples R China Tsinghua Univ, Ctr Astrophys, Beijing 10084, Peoples R China MIT, Kavli Inst Astrophys & Space Res, 77 Massachusetts Ave, Cambridge, MA 02139 USA Peking Univ, Sch Phys, Dept Astron, Beijing 100871, Peoples R China Max Planck Inst Astrophys, Karl Schwarzschild Str 1, D-85741 Garching, Germany Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA |
| Keywords | HALO OCCUPATION DISTRIBUTION QUENCHING TIME-SCALES DARK-MATTER HALOES STAR-FORMATION STELLAR MASS ILLUSTRISTNG SIMULATIONS COSMOLOGICAL SIMULATIONS DYNAMICAL FRICTION PLANCK COSMOLOGY SIZE EVOLUTION |
| Issue Date | Apr-2020 |
| Publisher | ASTROPHYSICAL JOURNAL |
| Abstract | Satellites constitute an important fraction of the overall galaxy population and are believed to form in dark matter subhalos. Here we use the cosmological hydrodynamic simulation TNG100 to investigate how the formation histories of subhalos affect the properties and evolution of their host galaxies. We use a scaled formation time (anf) to characterize the mass assembly histories of the subhalos before they are accreted by massive host halos. We find that satellite galaxies in young subhalos (low anf) are less massive and more gas-rich and have stronger star formation and a higher fraction of ex situ stellar mass than satellites in old subhalos (high a(nf)). Furthermore, these low-anf satellites require longer timescales to be quenched as a population than the high-anf counterparts. We find very different merger histories between satellites in fast-accretion (FA, a(nf) < 1.3) and slow-accretion (SA, a(nf) > 1.3) subhalos. For FA satellites the galaxy merger frequency dramatically increases just after accretion, which enhances the star formation at accretion, whereas for SA satellites the mergers occur smoothly and continuously across the accretion time. Moreover, mergers with FA satellites happen mainly after accretion, while a contrary trend is found for SA satellites. Our results provide insight into the evolution and star formation quenching of the satellite population. |
| URI | http://hdl.handle.net/20.500.11897/588597 |
| ISSN | 0004-637X |
| DOI | 10.3847/1538-4357/ab8464 |
| Indexed | SCI(E) Scopus |
| Appears in Collections: | 科维理天文与天体物理研究所 物理学院 |
