The size evolution of star-forming and quenched galaxies in the IllustrisTNG simulation

被引:228
作者
Genel, Shy [1 ,2 ]
Nelson, Dylan [3 ]
Pillepich, Annalisa [4 ]
Springel, Volker [5 ,6 ]
Pakmor, Ruediger [5 ]
Weinberger, Rainer [5 ]
Hernquist, Lars [7 ]
Naiman, Jill [7 ]
Vogelsberger, Mark [8 ]
Marinacci, Federico [8 ]
Torrey, Paul [8 ]
机构
[1] Flatiron Inst, Ctr Computat Astrophys, 162 Fifth Ave, New York, NY 10010 USA
[2] Columbia Univ, Columbia Astrophys Lab, 550 West 120th St, New York, NY 10027 USA
[3] Max Planck Inst Astrophys, Karl Schwarzschild Str 1, D-85740 Garching, Germany
[4] Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany
[5] Heidelberg Inst Theoret Studies, Schloss Wolfsbrunnenweg 35, D-69118 Heidelberg, Germany
[6] Heidelberg Univ, Zentrum Astron, ARI, Monchhofstr 12-14, D-69120 Heidelberg, Germany
[7] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA
[8] MIT, Dept Phys, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA
基金
欧洲研究理事会;
关键词
methods: numerical; galaxies: evolution; galaxies: formation; galaxies: structure; cosmology: theory; MASS ASSEMBLY GAMA; VELOCITY-DISPERSION EVOLUTION; DARK-MATTER HALOES; DIGITAL SKY SURVEY; STELLAR MASS; COMPACT GALAXIES; DISK GALAXIES; ELLIPTIC GALAXIES; EAGLE SIMULATION; MINOR MERGERS;
D O I
10.1093/mnras/stx3078
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
We analyse scaling relations and evolution histories of galaxy sizes in TNG100, part of the IllustrisTNG simulation suite. Observational qualitative trends of size with stellar mass, star formation rate and redshift are reproduced, and a quantitative comparison of projected r band sizes at 0 less than or similar to z less than or similar to 2 shows agreement to much better than 0.25 dex. We follow populations of z = 0 galaxies with a range of masses backwards in time along their main progenitor branches, distinguishing between main-sequence and quenched galaxies. Our main findings are as follows. (i) At M-*,M-z=0 greater than or similar to 10(9.5) M-circle dot, the evolution of the median main progenitor differs, with quenched galaxies hardly growing in median size before quenching, whereas main-sequence galaxies grow their median size continuously, thus opening a gap from the progenitors of quenched galaxies. This is partly because the main-sequence high-redshift progenitors of quenched z = 0 galaxies are drawn from the lower end of the size distribution of the overall population of main-sequence high-redshift galaxies. (ii) Quenched galaxies with M-*,(z=0) greater than or similar to 10(9.5) M-circle dot experience a steep size growth on the size-mass plane after their quenching time, but with the exception of galaxies with M-*,M-z=0 greater than or similar to 10(11) M-circle dot, the size growth after quenching is small in absolute terms, such that most of the size (and mass) growth of quenched galaxies (and its variation among them) occurs while they are still on the main sequence. After they become quenched, the size growth rate of quenched galaxies as a function of time, as opposed to versus mass, is similar to that of main-sequence galaxies. Hence, the size gap is retained down to z = 0.
引用
收藏
页码:3976 / 3996
页数:21
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