Quenching in cosmic sheets: tracing the impact of large-scale structure collapse on the evolution of dwarf galaxies

被引:13
作者
Pasha, Imad [1 ]
Mandelker, Nir [1 ,2 ,3 ,4 ]
van den Bosch, Frank C. [1 ]
Springel, Volker [5 ]
van de Voort, Freeke [6 ]
机构
[1] Yale Univ, Dept Astron, POB 208101, New Haven, CT 06511 USA
[2] Hebrew Univ Jerusalem, Racah Inst Phys, IL-91904 Jerusalem, Israel
[3] Univ Calif Santa Barbara, Kavli Inst Theoret Phys, Santa Barbara, CA 93106 USA
[4] Heidelberger Inst Theoret Studien, Schloss Wolfsbrunnenweg 35, D-69118 Heidelberg, Germany
[5] Max Planck Inst Astrophys, Karl Schwarzschild Str 1, D-85748 Garching, Germany
[6] Cardiff Univ, Cardiff Hub Astrophys Res & Technol, Queens Bldg, Cardiff CF243AA, Wales
基金
美国国家航空航天局; 美国国家科学基金会;
关键词
methods: numerical; galaxies: dwarf; galaxies: evolution; galaxies: high-redshift; intergalactic medium; galaxies: star formation; SMOOTHED PARTICLE HYDRODYNAMICS; STAR-FORMATION HISTORIES; COSMOLOGICAL SIMULATIONS; ILLUSTRISTNG SIMULATIONS; THERMAL INSTABILITIES; RED SEQUENCE; HALO MASS; CLUSTERS; ORIGIN; ENVIRONMENT;
D O I
10.1093/mnras/stac3776
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
Dwarf galaxies are thought to quench primarily due to environmental processes most typically occurring in galaxy groups and clusters or around single, massive galaxies. However, at earlier epochs, (5 < z < 2), the collapse of large-scale structure (forming Zel'dovich sheets and subsequently filaments of the cosmic web) can produce volume-filling accretion shocks which elevate large swaths of the intergalactic medium (IGM) in these structures to a hot (T > 10(6) K) phase. We study the impact of such an event on the evolution of central dwarf galaxies (5.5 < log M-* < 8.5) in the field using a spatially large, high resolution cosmological zoom simulation which covers the cosmic web environment between two protoclusters. We find that the shock-heated sheet acts as an environmental quencher much like clusters and filaments at lower redshift, creating a population of quenched, central dwarf galaxies. Even massive dwarfs that do not quench are affected by the shock, with reductions to their sSFR and gas accretion. This process can potentially explain the presence of isolated quenched dwarf galaxies, and represents an avenue of pre-processing, via which quenched satellites of bound systems quench before infall.
引用
收藏
页码:2692 / 2708
页数:17
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