Halo occupation numbers and galaxy bias

By J. Peacock, R. E. Smith. 2000

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We propose a heuristic model that displays the main features of realistic theories for galaxy bias. We first show that the low-order clustering statistics of the dark-matter distribution depend almost entirely on the locations and density profiles of dark-matter haloes. The quasi-linear mass correlations are in fact reproduced well by a model of independent randomly-placed haloes. The distribution of galaxies within the halo density field depends on: (i) the efficiency of galaxy formation, as manifested by the halo occupation number– the number of galaxies brighter than some sample limit contained in a halo of a given mass; (ii) the location of these galaxies within their halo. The first factor is constrained by the empirical luminosity function of groups. For the second factor, we assume that one galaxy marks the halo centre, with any remaining galaxies acting as satellites that trace the halo mass. This second assumption is essential if small-scale galaxy correlations are to remain close to a single power law, rather than flattening in the same way as the correlations of the overall density field. These simple assumptions amount to a recipe for non-local bias, in which the probability of finding a galaxy is not a simple function of its local mass density. We have applied this prescription to some CDM models of current interest, and find that the predictions are close to the observed galaxy correlations for a flat Ω=0.3 model (ΛCDM), but not for an Ω=1 model with the same power spectrum (τCDM). This is an inevitable consequence of cluster normalization for the power spectra: cluster-scale haloes of given mass have smaller core radii for high Ω, and hence display enhanced small-scale clustering. Finally, the pairwise velocity dispersion of galaxies in the ΛCDM model is lower than that of the mass, allowing cluster-normalized models to yield a realistic Mach number for the peculiar velocity field. This is largely due to the strong variation of galaxy-formation efficiency with halo mass that is required in this model.

Subfields: Astronomy and Astrophysics, Biophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/9641cdafc9bd95e86724b978950d0f4a1124b1a7

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Citations in the corpus

GAMA: towards a physical understanding of galaxy formation (2009, background): “Empirically, astronomers thus have to consider the halo occupation distribution: the number of galaxies hosted by a halo as a function of its mass and other properties (e.g. Peacock and Smith 2000, Berlind and Weinberg 2002).”
Galaxy Groups in the SDSS DR4. II. Halo Occupation Statistics (2007, methodology): “…has been extensively used to study the galaxy distribution in dark matter halos and galaxy clustering on large scales (e.g., Jing et al. 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 &…”
The effects of galaxy formation on the matter power spectrum: a challenge for precision cosmology (2011, methodology): “This method is based on concepts from the “halo model”, in which the density field is viewed as a distribution of isolated haloes (e.g. Peacock & Smith 2000; Seljak 2000; Cooray & Sheth 2002).”
Modelling galaxy clustering in a high-resolution simulation of structure formation (2006, background): “…HOD models are constructed by specifying the number of galaxies N that populate a dark matter halo of mass M as well as the distribution of galaxies within these haloes(Kauffmann et al. 1997; Peacock & Smith 2000; Seljak 2000; Benson et al. 2000; Berlind & Weinberg 2002; Berlind et al. 2003).”
Scaling relations for galaxy clusters in the Millennium-XXL simulation (2012, methodology): “In order to mimic this, we start by constructing a threedimensional galaxy catalogue using a halo occupation distribution (HOD) model (Kauffmann et al. 1997; Benson et al. 2000; Peacock & Smith 2000) to populate each MXXL halo with galaxies.”
EMU: Evolutionary Map of the Universe (2011, methodology): “EMUwill enable not only statistical approaches (e.g. halo occupation distribution modelling: Peacock & Smith 2000) but also directly observed overdensities using tracers such as WATs (Mao et al. 2010).”
NEW CONSTRAINTS ON THE EVOLUTION OF THE STELLAR-TO-DARK MATTER CONNECTION: A COMBINED ANALYSIS OF GALAXY–GALAXY LENSING, CLUSTERING, AND STELLAR MASS FUNCTIONS FROM z = 0.2 to z = 1 (2011, background): “…distribution P (N |Mh) that a halo of mass Mh is host to N galaxies above some threshold in luminosity or stellar mass (e.g., Seljak 2000; Peacock & Smith 2000; Scoccimarro et al. 2001; Berlind & Weinberg 2002; Bullock et al. 2002; Zehavi et al. 2002, 2005, 2011b; Zheng et al. 2005,…”
Galaxy Evolution from Halo Occupation Distribution Modeling of DEEP2 and SDSS Galaxy Clustering (2007, background): “…the framework of the Halo Occupation Distribution (HOD), which describes the statistical relation between galaxies and dark matter halos (see e.g., Jing, Mo, & Börner 1998; Ma & Fry 2000; Peacock & Smith 2000; Seljak 2000; Scoccimarro et al. 2001; Berlind & Weinberg 2002; Cooray & Sheth 2002).”
The Dark Side of the Halo Occupation Distribution (2003, background): “Moreover, it has been shown that a subPoisson P(N jM ) distribution is required in order to produce a correlation function of the observed power-law form (Benson et al. 2000b; Seljak 2000; Peacock & Smith 2000; Scoccimarro et al. 2001; Berlind & Weinberg 2002).”
Mapping stellar content to dark matter haloes using galaxy clustering and galaxy–galaxy lensing in the SDSS DR7 (2015, methodology): “…yzu@cmu.edu In this paper we develop a novel statistical approach within the Halo Occupation Distribution (HOD; Jing et al. 1998; Ma & Fry 2000; Peacock & Smith 2000; Seljak 2000; Yang et al. 2003; Scoccimarro et al. 2001; Cooray & Sheth 2002; Berlind & Weinberg 2002; Guzik & Seljak 2002;…”
Very Small Scale Clustering and Merger Rate of Luminous Red Galaxies (2005, background): “…of the correlation function from a power law on these scales can be interpreted in the framework of the halo occupation distribution (HOD; Peacock & Smith 2000; Seljak 2000; Scoccimarro et al. 2001; Berlind &Weinberg 2002) as a natural transition between galaxy pairs within a single…”
Resolving cosmic structure formation with the Millennium-II simulation (2009, background): “…‘two-halo’ contributions: on smaller scales the correlation function is dominated by dark matter particle pairs within the same halo, while on larger scales it is dominated by pairs in separate halos (Peacock & Smith 2000; Seljak 2000; Ma & Fry 2000; Scoccimarro et al. 2001; Cooray & Sheth 2002).”
The detectability of baryonic acoustic oscillations in future galaxy surveys. (2007, methodology): “The form of the HOD is constrained to reproduce a particular clustering measurement, such as the galaxy correlation function (e.g. Peacock & Smith 2000; Seljak 2000; Scoccimarro et al. 2001; Cooray & Sheth 2002).”
hmcode-2020: improved modelling of non-linear cosmological power spectra with baryonic feedback (2020, methodology): “The halo model (Seljak 2000; Peacock & Smith 2000) is just such a semi-analytical model of clustering.”
Cosmic evolution of quasar clustering: implications for the host haloes (2004, methodology): “These have been successfully used to describe the abundance and clustering properties of galaxies at both low (Peacock & Smith 2000; Seljak 2000; Scoccimarro et al. 2001; Berlind & Weinberg 2002; Marinoni & Hudson 2002; Magliocchetti & Porciani 2003; van den Bosch, Mo & Yang 2003; Yang, Mo & van…”
The clustering of Galaxies in the SDSS-III Baryon Oscillation Spectroscopic Survey: including covariance matrix errors (2013, methodology): “The halos were populated with mock galaxies using a Halo Occupation Distribution (HOD; Peacock & Smith 2000; Cooray & Sheth 2002; Berlind & Weinberg 2002) prescription, which was calibrated to reproduce the clustering measurements on scales between30 h−1 Mpc and80 h−1 Mpc. Mock catalogues were then…”
A halo model of galaxy colours and clustering in the Sloan Digital Sky Survey (2008, background): “…1998; Benson et al. 2000; Seljak 2000; Scoccimarro et al. 2001; Berlind & Weinberg 2002; Zehavi et al. 2005) the ‘conditional luminosity function’ (CLF; Peacock & Smith 2000; Yang et al. 2003; Cooray 2006; van den Bosch et al. 2007a), and the ‘subhalo abundance matching’ (SHAM; Klypin et al.…”
The dark side of galaxy colour (2013, background): “…e.g., Yang et al. 2003; van den Bosch et al. 2007)), which adopts parametric forms for the biased relation between galaxies and halo mass (e.g., Peacock & Smith 2000; Seljak 2000; Scoccimarro et al. 2001; Berlind & Weinberg 2002; Cooray & Sheth 2002; Zheng et al. 2007; Leauthaud et al. 2011;…”
GALAXY GROUPS IN THE SDSS DR4. III. THE LUMINOSITY AND STELLAR MASS FUNCTIONS (2008, methodology): “…has been extensively used to study the galaxy distribution in dark matter halos and galaxy clustering on large scales (e.g. Jing, Mo & Börner 1998; Peacock & Smith 2000; Seljak 2000; Scoccimarro et al. 2001; Jing, Börner & Suto 2002; Berlind & Weinberg 2002; Bullock, Wechsler & Somerville 2002;…”