The Halo Occupation Distribution and the Physics of Galaxy Formation

By A. Berlind, D. Weinberg, A. Benson, C. Baugh, Shaun Cole, R. Dav'e, Carlos S. Frenk, Adrian Jenkins, Neal Katz, C. Lacey. 2002

313 citations recorded by the source corpus.

The halo occupation distribution (HOD) describes the bias between galaxies and dark matter by specifying (1) the probability P(N|M) that a halo of virial mass M contains N galaxies of a particular class and (2) the relative spatial and velocity distributions of galaxies and dark matter within halos. We calculate and compare the HODs predicted by a smoothed particle hydrodynamics (SPH) simulation of a ΛCDM cosmological model (cold dark matter with a cosmological constant) and by a semianalytic galaxy formation model applied to the same cosmology. Although the two methods predict different galaxy mass functions, their HOD predictions for samples of the same space density agree remarkably well. In a sample defined by a baryonic mass threshold, the mean occupation function ⟨N⟩M exhibits a sharp cutoff at low halo masses, a slowly rising plateau in which ⟨N⟩ climbs from 1 to 2 over nearly a decade in halo mass, and a more steeply rising high-occupancy regime at high halo mass. In the low-occupancy regime, the factorial moments ⟨N(N - 1)⟩ and ⟨N(N - 1)(N - 2)⟩ are well below the values of ⟨N⟩2 and ⟨N⟩3 expected for Poisson statistics, with important consequences for the small-scale behavior of the two- and three-point correlation functions. The HOD depends strongly on galaxy age, with high-mass halos populated mainly by old galaxies and low-mass halos by young galaxies. The distribution of galaxies within SPH halos supports the assumptions usually made in semianalytic calculations: the most massive galaxy lies close to the halo center and moves near the halo's mean velocity, while the remaining, satellite galaxies have the same radial profile and velocity dispersion as the dark matter. The mean occupation at fixed halo mass in the SPH simulation is independent of the halo's larger scale environment, supporting both the merger tree approach of the semianalytic method and the claim that the HOD provides a complete statistical characterization of galaxy bias. We discuss the connections between the predicted HODs and the galaxy formation physics incorporated in the SPH and semianalytic approaches. These predictions offer useful guidance to theoretical models of galaxy clustering, and they will be tested empirically by ongoing analyses of galaxy redshift surveys. By applying the HODs to a large-volume N-body simulation, we show that both methods predict slight departures from a power-law galaxy correlation function, similar to features detected in recent observational analyses.

Subfields: Artificial Intelligence, Astronomy and Astrophysics, Global and Planetary Change

View Paper: https://www.semanticscholar.org/paper/d32a83aeecaf5a303f87d211f7a83a90089b2452

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Citations in the corpus

Assembly bias in the clustering of dark matter haloes (2006, background): “…galaxy clustering, namely that the galaxy content of a halo of given mass is statistically independent of its larger scale environment (e.g. Kauffmann, Nusser & Steinmetz 1997; Jing, Mo & Boerner 1998; Peacock & Smith 2000; Benson et al. 2000; Berlind et al. 2003; Yang, Mo & van den Bosch 2003).”
Linking halo mass to galaxy luminosity (2004, background): “The halo occupation distribution (HOD) model (Seljak 2000; Benson 2001; Berlind & Weinberg 2002; Bullock, Wechsler & Somerville 2002; Zheng et al. 2002; Berlind et al. 2003; Magliocchetti & Porciani 2003) is based on the probability P(N|M) that a halo of mass M is host to N galaxies.”
The Intermediate-Scale Clustering of Luminous Red Galaxies (2004, background): “…between halos (Kauffmann et al. 1997, 1999; Jing et al. 1998; Benson et al. 2000; Ma & Fry 2000; Peacock & Smith 2000; Seljak 2000; Scoccimarro et al. 2001; Berlind & Weinberg 2002; Berlind et al. 2003; Magliocchetti & Porciani 2003; Kravtsov et al. 2004; Zehavi et al. 2004a; Zheng 2004).”
The age dependence of halo clustering (2005, background): “…mass halos, while assuming the galaxy population in a halo of given mass to be independent of where the halo lies (e.g. Kauffmann, Nusser & Steinmetz 1997; Jing, Mo & Börner, 1998; Benson et al 2000; Peacock & Smith 2000; Wechsler et al 2001; Berlind et al 2003; van den Bosch, Yang & Mo 2003).”
THE GALAXY CONTENT OF SDSS CLUSTERS AND GROUPS (2007, background): “Furthermore, the flattening and “saturating” of the red fraction for the most massive systems appears to be a natural product of modeling (Berlind et al. 2003; Zheng et al. 2005).”
Galaxy Groups in the SDSS DR4. II. Halo Occupation Statistics (2007, background): “…1998, 2002; Peacock & Smith 2000; Seljak 2000; Scoccimarro et al. 2001; Berlind & Weinberg 2002; Bullock et al. 2002; Scranton 2002; Kang et al. 2002; Marinoni & Hudson 2002; Zheng et al. 2002, 2005; Magliocchetti & Porciani 2003; Berlind et al. 2003; Zehavi et al. 2004, 2005; Tinker et al. 2005).”
The Luminosity and Color Dependence of the Galaxy Correlation Function (2004, methodology): “…a cosmological constant) with parameters motivated by independent measurements, and we adopt parameterized forms of the HOD loosely motivated by contemporary theories of galaxy formation (Kauffmann et al. 1997, 1999; Benson et al. 2000; Berlind et al. 2003;Kravtsov et al. 2004; Zheng et al. 2004).”
Properties of galaxy groups in the Sloan Digital Sky Survey – I. The dependence of colour, star formation and morphology on halo mass (2005, background): “Berlind et al. (2003) and Zheng et al. (2005) have shown that the semi-analytical models of Cole et al. (2000) predict that the fraction of ‘young’ galaxies decreases with increasing halo mass up to ∼1013 h−1 M , after which the fraction remains constant.”
Forecasting cosmological constraints from redshift surveys (2008, background): “Simulations suggest little or no velocity bias for the majority of “galaxies” in dark matter (Springel et al. 2001; Faltenbacher et al. 2006) and hydrodynamic (Berlind et al. 2003) simulations atthe same level.”
CLASH-VLT: The mass, velocity-anisotropy, and pseudo-phase-space density profiles of the z = 0.44 galaxy cluster MACS J1206.2-0847 (2013, background): “Numerical simulations suggest that a bias exists, albeit small (e.g. Berlind et al. 2003; Biviano et al. 2006; Munari et al. 2013), so we must take this result with caution.”
Galaxy evolution in cosmological simulations with outflows ― I. Stellar masses and star formation rates (2011, background): “For M∗ > M ⋆ the satellite fraction decreases, although it is high again at very large masses – these are satellites in galaxy groups where the halo occupation distribution is steeply rising (e.g. Berlind et al. 2003).”
Theoretical Models of the Halo Occupation Distribution: Separating Central and Satellite Galaxies (2004, background): “…of galaxy formation theory (e.g., Kauffmann, Nusser, & Steinmetz 1997; Kauffmann et al. 1999; Benson et al. 2000; White, Hernquist, & Springel 2001; Yoshikawa et al. 2001; Berlind et al. 2003; Kravtsov et al. 2004), which can be tested by deriving the HOD empirically from observed clustering.”
Cosmological constraints from a combination of galaxy clustering and lensing – I. Theoretical framework (2012, methodology): “Although this makes it difficult to calibrate galaxy formation models using halo occupation statistics (e.g., Berlind et al. 2003), it also implies that one can use this method to constrain cosmological parameters as long as one has some independent constraints on halo occupation statistics.”
A marked correlation function analysis of halo formation times in the Millennium Simulation (2005, unknown): “…the properties of the galaxy population depend sufficiently strongly on the merger history of a halo, we see that this assumption is no longer strictly valid, and this t erefore calls into question the validity of results based on this formalism (e.g., Berlind et al. 2003; Abazajian et al. 2005).”
A halo-based galaxy group finder: calibration and application to the 2dFGRS (2004, background): “…halo resides at rest at the centre, while the number density distribution of the fainter, satellite galaxies matches that of the dark matter particles (e.g., Carlberg et al. 1997; van der Marel et al. 2000; Berlind et al. 2003; Lin, Mohr & Stanford 2004; Rines et al. 2004; Diemand et al. 2004).”
The Dark Side of the Halo Occupation Distribution (2003, methodology): “This is supported both by theoretical models (Berlind et al. 2003 and references therein) and by halo model fits to observational data (e.g., Scoccimarro et al. 2001; Zehavi et al. 2003; Magliocchetti & Porciani 2003).”
Semianalytical Model of Galaxy Formation with High-Resolution N-Body Simulations (2004, methodology): “Another powerful tool to link galaxies to dark matter halos is the so-called halo occupation model (Yang et al. 2003b; van den Bosch et al. 2003; Berlind et al. 2003; Zheng et al. 2005; Vale & Ostriker 2004; Kravtsov et al. 2004; for earlier work, see Jing et al. 1998; Peacock & Smith 2000; Seljak…”