The dependence of halo clustering on halo formation history, concentration, and occupation

被引:463
作者
Wechsler, Risa H.
Zentner, Andrew R.
Bullock, James S.
Kravtsov, Andrey V.
Allgood, Brandon
机构
[1] Univ Chicago, Dept Astron & Astrophys, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA
[2] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA
[3] Univ Calif Irvine, Dept Phys & Astron, Ctr Cosmol, Irvine, CA 92697 USA
[4] Univ Calif Santa Cruz, Dept Phys, Santa Cruz, CA 96050 USA
基金
美国国家科学基金会;
关键词
cosmology : theory; dark matter; galaxies : formation; galaxies : halos; large-scale structure of universe; methods : numerical;
D O I
10.1086/507120
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
We investigate the dependence of dark matter halo clustering on halo formation time, density profile concentration, and subhalo occupation number, using high-resolution numerical simulations of a Lambda CDM cosmology. We confirm results that halo clustering is a function of halo formation time at fixed mass and that this trend depends on halo mass. For the first time, we show unequivocally that halo clustering is a function of halo concentration and show that the dependence of halo bias on concentration, mass, and redshift can be accurately parameterized in a simple way: b(M; c vertical bar z) b(M vertical bar z)b(cvir) (c vertical bar M/M*). Interestingly, the scaling between bias and concentration changes sign with the value of M/M*: high-concentration (early forming) objects cluster more strongly for M less than or similar to M*, while low- concentration (late forming) objects cluster more strongly for rare high- mass halos, M greater than or similar to M*. We show the first explicit demonstration that host dark halo clustering depends on the halo occupation number (of dark matter subhalos) at fixed mass and discuss implications for halo model calculations of dark matter power spectra and galaxy clustering statistics. The effect of these halo properties on clustering is strongest for early- forming dwarf- mass halos, which are significantly more clustered than typical halos of their mass. Our results suggest that isolated low-mass galaxies (e.g. low surface brightness dwarfs) should have more slowly rising rotation curves than their more clustered counterparts and may have consequences for the dearth of dwarf galaxies in voids. They also imply that self-calibrating richness-selected cluster samples with their clustering properties might overestimate cluster masses and bias cosmological parameter estimation.
引用
收藏
页码:71 / 84
页数:14
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