The Physics of Galaxy Clustering. I. A Model for Subhalo Populations

By A. Zentner, A. Berlind, James S. Bullock, Andrey V. Kravtsov, Risa Wechsler. 2004

285 citations recorded by the source corpus.

We present a semianalytic model for cold dark matter halo substructure that can be used as a framework for studying the physics of galaxy formation and as an ingredient in halo models of galaxy clustering. The model has the following main ingredients: (1) extended Press-Schechter mass accretion histories, (2) host halo density profiles computed according to the trends observed in cosmological simulations, (3) distributions of initial orbital parameters of accreting subhalos measured in a high-resolution simulation of three Milky Way-size halos, and (4) integration of the orbital evolution of subhalos including the effects of dynamical friction and tidal mass loss. We perform a comprehensive comparison of the model calculations to the results of a suite of high-resolution cosmological simulations. The comparisons show that subhalo statistics such as the velocity and mass functions, the radial distributions, and the halo occupation distributions agree well over 3 orders of magnitude in host halo mass and at various redshifts. We find that both in the simulations and in our model the radial distributions of subhalos are significantly shallower than that of the dark matter density. The abundance of subhalos in a host is set by competition between tidal disruption and new accretion. Halos of high mass and halos at high redshift tend to host more subhalos because the subhalos have, on average, been accreted more recently. Similarly, at a fixed mass and epoch, halos that formed more recently host a larger number of subhalos. Observed "fossil groups" may represent an extreme tail of this correlation. We find a related correlation between host halo concentration and satellite abundance at fixed host mass, Nsat ∝ c, where a changes with redshift and host-to-subhalo mass ratio. Lastly, we use our substructure model to populate host halos in one of the high-resolution cosmological simulations, replacing the actual subhalos resolved in this simulation and using the host mass as the only input for the model calculation. We show that the resulting correlation function of such a hybrid halo ensemble is indistinguishable from that measured directly in the simulation. This supports one of the key tenets of the standard halo model, i.e., the assumption that the halo occupation distribution is statistically independent of the host halo environment.

Subfields: Astronomy and Astrophysics, Ecology, Instrumentation

View Paper: https://www.semanticscholar.org/paper/c868b764c22211e6af7fe189752cce0e41900a2b

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Citations in the corpus

A QUANTITATIVE EXPLANATION OF THE OBSERVED POPULATION OF MILKY WAY SATELLITE GALAXIES (2009, result): “This simple analytic model is able to reproduce the sub-halo mass function, in reasonably good agreement with that found in numerical N -body simulations (Zentner et al. 2005; Shaw et al. 2006; Yoo et al. 2007).”
What determines satellite galaxy disruption (2009, background): “Zentner et al. (2005) and Taylor & Babul (2004) consider a satellite subhalo to be tidally disrupted when the mass of the subhalo has been stripped to a value less than the mass within adisrs, where rs is the subhalo’s NFW (Navarro et al. 1996) scale radius at infall, with adis = 1 (Zentner et al.…”
Galaxy assembly bias: a significant source of systematic error in the galaxy–halo relationship (2013, background): “Effect (ii) can be understood in terms of merging and tidal disruption of subhalos (see, for example, Figure 14 of Zentner et al. 2005).”
HALO OCCUPATION DISTRIBUTION MODELING OF CLUSTERING OF LUMINOUS RED GALAXIES (2008, background): “The decrease of the scaling factor reflects the balance between accretion and destruction of satellites (Zentner et al. 2005)— massive halos assemble more recently and their satellites have less time to merge with the central galaxy.”
Thin, thick and dark discs in ΛCDM (2008, background): “Similar results have been derived previously from semi-analytic models (Taylor & Babul 2001, 2004, 2005; Zentner & Bullock 2003; Zentner et al. 2005).”
The shape of dark matter haloes : dependence on mass, redshift, radius and formation (2005, methodology): “…with masses above M ∗ to be undergoing a higher rate of merging than haloes with masses below M ∗, and because it has been shown that this merging happens along preferred directions (Knebe et al. 2004; Faltenbacher et al. 2005; Zentner et al. 2005), the prolateness is most likely due to merging.”
A Cosmological Framework for the Co-Evolution of Quasars, Supermassive Black Holes, and Elliptical Galaxies. I. Galaxy Mergers and Quasar Activity (2007, methodology): “For each halo, we calculate the (weakly mass- and redshift-dependent) subhalo mass function (or distribution of subhalos, P½NsubhalojMsubhalo;Mhalo ) following Zentner et al. (2005) and Kravtsov et al. (2004).”
DISSIPATION AND EXTRA LIGHT IN GALACTIC NUCLEI. IV. EVOLUTION IN THE SCALING RELATIONS OF SPHEROIDS (2008, methodology): “For each halo, we calculate the (weakly mass and redshift dependent) subhalo mass function (or distribution of subhalos,P[Nsubhalo|Msubhalo, Mhalo]) following Zentner et al. (2005) and Kravtsov et al. (2004).”
Formation and Evolution of Galaxy Dark Matter Halos and Their Substructure (2007, background): “This nearly constant substructure abundance over the last 5 Gyrs seems to be at odds with the recently found trends that old virialized systems are less clumpy (Gao et al. 2004; van den Bosch et al. 2005; Zentner et al. 2005).”
Galaxy Evolution from Halo Occupation Distribution Modeling of DEEP2 and SDSS Galaxy Clustering (2007, methodology): “If we know the halo occupation as a function of stellar mass at z ∼ 1, we can evolve the subhalo and halo population at z ∼ 1 to z ∼ 0 using high resolution N -body simulation or analytic code (e.g., Zentner et al. 2005), assuming no star formation.”
EVOLUTION OF THE GALAXY–DARK MATTER CONNECTION AND THE ASSEMBLY OF GALAXIES IN DARK MATTER HALOS (2011, background): “2(1− η)1.2 , (19) independent of redshift or halo mass (e.g., Zentner et al. 2005).”
Merger Histories of Galaxy Halos and Implications for Disk Survival (2007, background): “3 Gyr for typical orbital parameters (Boylan-Kolchin et al. 2007; Zentner et al. 2005; Zentner & Bullock 2003).”
A Fitting Formula for the Merger Timescale of Galaxies in Hierarchical Clustering (2007, methodology): “Various authors (e.g., Tormen 1997; Zentner et al. 2005; Khochfar & Burkert 2006) have studied this distribution, with similar conclusions that orbits with intermediate ǫ are common while those at both ends (ǫ ≈ 0 or 1) are rare.”
The effect of galaxy mass ratio on merger-driven starbursts (2007, background): “The resulting interactions are fast and nearly radial, consistent with orbits found for dark matter halos in cosmological simulations (Vitvitska et al. 2002; Khochfar & Burkert 2006; Benson 2005; Zentner et al. 2005).”
Structure finding in cosmological simulations: the state of affairs (2013, background): “…1996; Smith et al. 2003), environmental effects (Baugh, Cole & Frenk 1996; Moore, Katz & Lake 1996), merger rates (Lacey & Cole 1994; Bower et al. 2006; Fakhouri & Ma 2008; Fakhouri, Ma & Boylan-Kolchin 2010; Behroozi et al. 2013c), disruption timescales (Ghigna et al. 1998; Zentner et al. 2005b).”
A Cosmological Framework for the Co-Evolution of Quasars, Supermassive Black Holes, and Elliptical Galaxies. II. Formation of Red Ellipticals (2007, methodology): “We therefore repeatmost of our calculations adopting both our ‘‘default’’subhalomass function calculation (Zentner et al. 2005; Kravtsov et al. 2004) and an alternative subhalo mass function calculation (van den Bosch et al. 2005, normalized to match cosmological simulations as in Shaw et al.…”
The Dependence of Halo Clustering on Halo Formation History, Concentration, and Occupation (2005, methodology): “…halos that accrete their subhalos first have more time for those subhalos to be destroyed or to merge with the central object due to dynamical friction (e.g., Kravtsov &Klypin 1999; Taffoni et al. 2003; Zentner & Bullock 2003; Zentner et al. 2005; van den Bosch et al. 2005; Taylor & Babul 2005).”
The Non-Parametric Model for Linking Galaxy Luminosity with Halo/Subhalo Mass: Are First Brightest Galaxies Special? (2005, methodology): “The slope α = 1.9 is set to the same value as is generally found for the present day subhalo mass function in simulations (e.g., Gao et al. 2004; Weller et al. 2005; van den Bosch, Tormen & Giocoli 2005; Zentner et al. 2005; Shaw et al. 2006).”