The subhalo populations of ΛCDM dark haloes

By Liang Gao, Simon D. M. White, Adrian Jenkins, Felix Stoehr, Volker Springel. 2004

540 citations recorded by the source corpus.

We investigate the subhalo populations of dark matter haloes in the concordance �CDM cosmology. We use a large cosmological simulation and a variety of high resolution resimulations of individual cluster and galaxy haloes to study the systematics of subhalo populations over ranges of 1000 in halo mass and 1000 in the ratio of subhalo to parent halo mass. The subhalo populations of different haloes are not scaled copies of each other, but vary systematically with halo properties. On average, the amount of substructure increases with halo mass. At fixed mass, it decreases with halo concentration and with halo formation redshift. These trends are comparable in size to the scatter in subhalo abundance between similar haloes. Averaged over all haloes of given mass, the abundance of low mass subhaloes per unit parent halo mass is independendent of parent mass. It is very similar to the abundance per unit mass of low mass haloes in the universe as a whole, once differing boundary definitions for subhaloes and haloes are accounted for. The radial distribution of subhaloes within their parent haloes is substantially less centrally concentrated than that of the dark matter. It varies at most weakly with the mass (or concentration) of the parent halo and not at all with subhalo mass. It does depend on the criteria used to define the subhalo population considered. About 90 per cent of present-day subhaloes were accreted after z = 1 and about 70 per cent after z = 0.5. Only about 8 per cent of the total mass of all haloes accreted at z = 1 survives as bound subhaloes at z = 0. For haloes accreted at z = 2, the survival mass fraction is just 2 per cent. Subhaloes seen near the centre of their parent typically were accreted earlier and retain less of their original mass than those seen near the edge. These strong systematics mean that comparison with galaxies in real clusters is only possible if the formation of the luminous component is modelled appropriately.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/0d740b306a0b94a849a13a10317e577f1ce676ed

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

In Instrumentation

Citations in the corpus

The Milky Way’s bright satellites as an apparent failure of ΛCDM (2011, methodology): “The substructure abundance in within the virial radii of dark matter halos is essentially self-similar when measured in terms of Vmax/Vvir (e.g., Gao et al. 2004; De Lucia et al. 2004; van den Bosch et al. 2005; Gao et al. 2011), and the cumulative abundance of dark matter subhalos in a given halo…”
MERGERS AND BULGE FORMATION IN ΛCDM: WHICH MERGERS MATTER? (2009, background): “Alternative subhalo mass functions from e.g. De Lucia et al. (2004); Gao et al. (2004); Nurmi et al. (2006) are consistent.”
Disruption of Dark Matter Substructure: Fact or Fiction? (2017, background): “…large cosmological simulations routinely resolve an entire hierarchy of substructure, with haloes hosting subhaloes, which themselves host sub-subhaloes, etc. (e.g., Ghigna et al. 1998; Tormen et al. 1998; Diemand et al. 2004a; Gao et al. 2004; Kravtsov et al. 2004; Giocoli et al. 2008a, 2010).”
Thin, thick and dark discs in ΛCDM (2008, result): “Our results for the surviving subhaloes agree well with previous studies (Gao et al. 2004; Ludlow et al. 2008) and have cumulative vmax functions well fit by their fitting function: N (> vmax) = A ( vmax vhostmax )−α , (1) where vhostmax is the peak circular speed of the host galaxy; α = 2.559 and…”
Galaxy evolution in groups and clusters: satellite star formation histories and quenching time-scales in a hierarchical Universe (2012, background): “Finally, trend (3) implies an evolutionary trend, because a satellite’s halo-centric radius negatively correlates with its time since infall (e.g., Gao et al. 2004; De Lucia et al. 2012).”
The properties of warm dark matter haloes (2013, background): “However, the number of subhaloes above a given mass or Vmax depends, of course, on the host halo mass (Gao et al. 2004; Wang et al. 2012).”
Co-orbiting satellite galaxy structures are still in conflict with the distribution of primordial dwarf galaxies (2014, result): “This is in conflict with the findings by Gao et al. (2004), accordingto which about 90 per cent of the present-day sub-haloes in cosmol gical simulations have been accreted afterz= 1.”
The stellar halo of the Galaxy (2008, background): “For comparison, satellite substructures around halos in dark matter cosmological simulations tend to be much more evenly distributed (Gao et al. 2004; Kang et al. 2005).”
Galaxy growth in the concordance ΛCDM cosmology (2007, background): “RAS vive as long-lived substructure within the larger objects by which they are accreted (Ghigna et al. 1998; Moore et al. 1999; Gao et al. 2004).”
The hierarchical formation of the brightest cluster galaxies (2006, background): “In recent work, Gao et al. (2004a) used numerical simulations to study the formation of the inner cores of massive dark matter haloes.”
The many manifestations of downsizing: hierarchical galaxy formation models confront observations (2009, methodology): “The WDL08 model explicitly follows DM substructures in the N-body simulation until tidal truncation and stripping reduce their mass below the resolution limit of the simu- lation (De Lucia et al. 2004a; Gao et al. 2004).”
The formation history of elliptical galaxies (2005, background): “This implies that the cluster– centric distance of the galaxies is correlated with the time they were accreted onto a larger structure (Diaferio et al. 2001; Gao et al. 2004).”
The importance of satellite quenching for the build-up of the red sequence of present-day galaxies (2007, result): “This is in accord with the fact that the present-day population of massive subhaloes (which host the massive satellite galaxies) fell into their parent halo fairly recently (Zentner & Bullock 2003; Gao et al. 2004; van den Bosch, Tormen & Giocoli 2005).”
Measurement of Galaxy Cluster Sizes, Radial Profiles, and Luminosity Functions from SDSS Photometric Data (2004, background): “…any population of galaxies in a host halo, the radial distribution is dependent on the dynamical and star formation histories of the galaxies once they enter the host halo, and may depend sensitively on how the population is selected (Diemand et al. 2004; Gao et al. 2004; Nagai & Kravtsov 2004).”
Orbital parameters of infalling dark matter substructures (2004, background): “…much work conducted in which the distribution and properties of substructures, their effects on galaxy disks and so on were examined (Ghigna et al. 1998; Tormen, Diaferio & Syer 1998; van den Bosch et al. 1999; Zhang et al. 2002; Benson et al. 2004; Gao et al. 2004; Diemand, Moore & Stadel 2004).”
Local-Group tests of dark-matter concordance cosmology - Towards a new paradigm for structure formation (2010, background): “ForMvir > 0.01Mh, the mass function steepens (Gao et al. 2004), so that it is effectively cut off at a massMmax (see Eq.”