How Many Galaxies Fit in a Halo? Constraints on Galaxy Formation Efficiency from Spatial Clustering

By R. Scoccimarro, R. Sheth, L. Hui, B. Jain. 2000

565 citations recorded by the source corpus.

We study galaxy clustering in the framework of halo models, where gravitational clustering is described in terms of dark matter halos. At small scales, dark matter clustering statistics are dominated by halo density profiles, whereas at large scales, correlations are the result of combining nonlinear perturbation theory with halo biasing. Galaxies are assumed to follow the dark matter profiles of the halo they inhabit, and galaxy formation efficiency is characterized by the number of galaxies that populate a halo of given mass. This approach leads to generic predictions: the galaxy power spectrum shows a power-law behavior even though the dark matter does not, and the galaxy higher order correlations show smaller amplitudes at small scales than their dark matter counterparts. Both are in qualitatively agreement with measurements in galaxy catalogs. We find that requiring the model to fit both the second- and third-order moments of the Automatic Plate Measuring Facility (APM) galaxies provides a strong constraint on galaxy formation models. The data at large scales require that galaxy formation be relatively efficient at small masses, m ≈ 1010 M☉ h-1, whereas data at smaller scales require that the number of galaxies in a halo scale approximately as the mass to the 0.8th power in the high-mass limit. These constraints are independent of those derived from the luminosity function or Tully-Fisher relation. We also predict the power spectrum, bispectrum, and higher order moments of the mass density field in this framework. Although halo models agree well with measurements of the mass power spectrum and the higher order Sp parameters in N-body simulations, the model assumption that halos are spherical leads to disagreement in the configuration dependence of the bispectrum at small scales. We stress the importance of finite-volume effects in higher order statistics and show how they can be estimated in this approach.

Subfields: Astronomy and Astrophysics, Instrumentation, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/f352bd21ec632b321259e99755c039d54c26e458

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

In Nuclear and High Energy Physics

Citations in the corpus

K-Band Properties of Galaxy Clusters and Groups: Luminosity Function, Radial Distribution, and Halo Occupation Number (2004, methodology): “The recent advent of the so-called halo model has introduced an important new tool for investigating this subject (e.g., Seljak 2000; Peacock & Smith 2000; Scoccimarro et al. 2001).”
Very Small Scale Clustering and Merger Rate of Luminous Red Galaxies (2005, background): “…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 virialized halo and galaxy pairs in…”
The MICE Grand Challenge lightcone simulation – II. Halo and galaxy catalogues (2013, methodology): “We have used a new hybrid technique that combines halo occupation distribution (HOD; e.g. Jing, Mo & Boerner 1998; Scoccimarro et al. 2001; Berlind & Weinberg 2002) and halo abundance matching (HAM; e.g. Tasitsiomi et al. 2004; Vale & Ostriker 2004; Conroy, Wechsler & Kravtsov 2006) prescriptions.”
The Halo Occupation Distribution and the Physics of Galaxy Formation (2002, methodology): “Benson et al. (2000b) and BW show that a sub-Poisson PðNjhNiÞ distribution makes it much easier to produce a correlation function of the observed power-law form; the alternative is to put galaxies into halos of implausibly low mass (see also Seljak 2000; Peacock & Smith 2000; Scoccimarro et al. 2001”
The Mass-to-Light Function of Virialized Systems and the Relationship between Their Optical and X-Ray Properties (2001, background): “Once this function is known, one can use the well-understood clustering of halos to obtain the clustering of galaxies (Neyman, Scott and Shane 1953; Kauffmann et al. 1999; Diaferio et al. 1999; Benson et al. 2000; Seljak 2000; Peacock and Smith 2000; Scoccimarro et al. 2001; Benson 2001).”
AN EMPIRICAL CHARACTERIZATION OF EXTENDED COOL GAS AROUND GALAXIES USING Mg ii ABSORPTION FEATURES (2010, methodology): “In Tinker & Chen (2008), we have introduced a novel technique that adopts the halo occupation framework (e.g. Seljak 2000; Scoccimarro et al. 2001; Berlind & Weinberg 2002) and characterizes the origin of QSO absorption-line systems based on a conditional mass function of dark matter halos in which…”
Clustering of intermediate redshift quasars using the final SDSS III-BOSS sample (2015, background): “…for instance, empirical approaches such as the halo occupation distribution framework (HOD; Seljak 2000; Peacock & Smith 2000; Benson et al. 2000; Scoccimarro et al. 2001; White, Hernquist & Springel 2001; Berlind & Weinberg 2002; Cooray & Sheth 2002, and references therein) have been successful…”
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…”
Detection of the Baryon Acoustic Peak in the Large-Scale Correlation Function of SDSS Luminous Red Galaxies (2005, methodology): “…mock catalogs are constructed using PTHalos (Scoccimarro & Sheth 2002) with a halo occupation model (Ma & Fry 2000; Seljak 2000; Peacock & Smith 2000; Scoccimarro et al. 2001; Cooray & Sheth 2002; Berlind et al. 2003) that matches the observed amplitude of clustering of LRGs (Zehavi et al. 2004a).”
A halo model of galaxy colours and clustering in the Sloan Digital Sky Survey (2008, methodology): “…rather different ways, which have come to be known as the ‘halo occupation distribution’ (HOD; Jing, Mo & Börner 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…”
Constraining galaxy formation and cosmology with the conditional luminosity function of galaxies (2002, background): “…study the bias and various other clustering statistics of the galaxy distribution (e.g., Jing, Mo & Börner 1998; Peacock & Smith 2000; Seljak 2000; Scoccimarro et al. 2001; White 2001; Jing, Börner & Suto 2002; Berlind & Weinberg 2002; Bullock, Wechsler & Somerville 2002; Scranton 2002; Kang et…”
GALAXY GROUPS IN THE SDSS DR4. III. THE LUMINOSITY AND STELLAR MASS FUNCTIONS (2008, background): “…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; Scranton 2002; Zehavi et al. 2004,…”
The impact of non‐Gaussian errors on weak lensing surveys (2008, methodology): “In this paper, we employ the dark matter halo approach (Seljak 2000; Peacock & Smith 2000; Ma & Fry 2000; Scoccimarro et al. 2001; also see Cooray & Sheth 2002 for a review), where then-point correlations of the mass distribution are modeled interms of two separate contributions: correlation of…”
The Dark Side of the Halo Occupation Distribution (2003, methodology): “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).”
A halo-based galaxy group finder: calibration and application to the 2dFGRS (2004, methodology): “…have used such halo occupation models to study various aspects of galaxy clustering (Jing, Mo & Börner 1998; Peacock & Smith 2000; Seljak 2000; Scoccimarro et al. 2001; White 2001; Jing, Börner & Suto 2002; Bullock, Wechsler & Somerville 2002; Berlind & Weinberg 2002; Scranton 2002; Kang et…”
Towards a concordant model of halo occupation statistics (2006, background): “Journal compilation C© 2007 RAS 2000; Scoccimarro et al. 2001; Berlind & Weinberg 2002; Cooray & Sheth 2002; Kang et al. 2002; Berlind et al. 2003).”