Mini-quenching of z=4-8 galaxies by bursty star formation

被引:35
作者
Dome, Tibor [1 ,2 ]
Tacchella, Sandro [2 ,3 ]
Fialkov, Anastasia [1 ,2 ]
Ceverino, Daniel [4 ,5 ]
Dekel, Avishai [6 ,7 ]
Ginzburg, Omri [6 ]
Lapiner, Sharon [6 ]
Looser, Tobias J. [2 ,3 ]
机构
[1] Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 0HA, England
[2] Kavli Inst Cosmol, Madingley Rd, Cambridge CB3 0HA, England
[3] Univ Cambridge, Cavendish Lab, 19 JJ Thomson Ave, Cambridge CB3 0HE, England
[4] Univ Autonoma Madrid, Fac Ciencias, Dept Fis Teor, Modulo 8, E-28049 Madrid, Spain
[5] Univ Autonoma Madrid, Fac Ciencias, CIAFF, E-28049 Madrid, Spain
[6] Hebrew Univ Jerusalem, Racah Inst Phys, Ctr Astrophys & Planetary Sci, IL-91904 Jerusalem, Israel
[7] Univ Calif Santa Cruz, SCIPP, Santa Cruz, CA 95064 USA
基金
英国科学技术设施理事会; 以色列科学基金会;
关键词
methods: numerical; galaxies: evolution; galaxies: formation; galaxies: high-redshift; galaxies: photometry; FORMATION MAIN-SEQUENCE; MASSIVE QUIESCENT GALAXIES; BLACK-HOLE FEEDBACK; FORMATION HISTORIES; H-ALPHA; FORMING GALAXIES; FORMATION VARIABILITY; LUMINOSITY FUNCTION; JWST PREDICTIONS; MESA ISOCHRONES;
D O I
10.1093/mnras/stad3239
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
The recent reported discovery of a low-mass z = 5.2 and an intermediate-mass z = 7.3 quenched galaxy with JWST/NIRSpec is the first evidence of halted star formation above z approximate to 5. Here, we show how bursty star formation at z = 4-8 gives rise to temporarily quenched, or mini-quenched galaxies in the mass range M-star = 10(7)-10(9) M-circle dot using four models of galaxy formation: the periodic box simulation ILLUSTRISTNG, the zoom-in simulations VELA and FIRSTLIGHT and an empirical halo model. The main causes for mini-quenching are stellar feedback, lack of gas accretion onto galaxies, and galaxy-galaxy interactions. The abundance of (mini-)quenched galaxies agrees across the models: the population first appears below z approximate to 8, after which their proportion increases with cosmic time, from similar to 0.5-1.0 per cent at z = 7 to similar to 2-4 per cent at z = 4, corresponding to comoving number densities of similar to 10(-5) and similar to 10(-3) Mpc(-3), respectively. These numbers are consistent with star formation rate duty cycles inferred for VELA and FIRSTLIGHT galaxies. Their star formation histories (SFHs) suggest that mini-quenching at z = 4-8 is short-lived with a duration of similar to 20-40 Myr, which is close to the free-fall time-scale of the inner halo. However, mock spectral energy distributions of mini-quenched galaxies in ILLUSTRISTNG and VELA do not match JADES-GS-z7-01-QU photometry, unless their SFHs are artificially altered to be more bursty on time-scales of similar to 40 Myr. Studying mini-quenched galaxies might aid in calibrating sub-grid models governing galaxy formation, as these may not generate sufficient burstiness at high redshift to explain the SFH inferred for JADES-GS-z7-01-QU.
引用
收藏
页码:2139 / 2151
页数:13
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