Analytic model for galaxy and dark matter clustering

By Uros Seljak. 2000

965 citations recorded by the source corpus.

We investigate an analytic model to compute the non-linear power spectrum of dark matter, galaxies and their cross-correlation. The model is based on Press–Schechter haloes, which cluster and have realistic dark matter profiles. The total power spectrum is a sum of two contributions, one from correlations between the haloes and one from correlations within the same halo. We show that such a model can give dark matter power spectra which match well with the results of N-body simulations, provided that the concentration parameter decreases with the halo mass. The galaxy power spectrum differs from the dark matter power spectrum because the pair-weighted number of galaxies does not scale with the halo mass and because most haloes harbour a central galaxy. If the pair-weighted number of galaxies increases less rapidly than the halo mass, as predicted by theoretical models and observed in clusters, then the resulting power spectrum becomes a power law with a slope close to the observed over several orders of magnitude in scale. Such a model also predicts a later onset of non-linear clustering in comparison with dark matter, which is needed to reconcile the cold dark matter (CDM) models with the data. A generic prediction of this model is that bias is scale-dependent and non-monotonic. This is particularly important for red or elliptical galaxies, which are preferentially found in larger mass haloes and for which the bias in the power spectrum may be scale-dependent even on large scales. Our predictions for galaxy–dark matter correlations, which can be observed through galaxy–galaxy lensing, show that these cannot be interpreted simply as an average halo profile of a typical galaxy, because different halo masses dominate at different scales and because larger haloes host more than one galaxy. We compute predictions for the cross-correlation coefficient as a function of scale and discuss the prospects of using cross-correlations in combination with galaxy clustering to determine the dark matter power spectrum.

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

View Paper: https://www.semanticscholar.org/paper/ca7a754055339052395bdfa90ae3ecdb251fa42a

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Citations in the corpus

The Luminosity and Color Dependence of the Galaxy Correlation Function (2004, methodology): “To achieve the accuracy needed to model the SDSS data, we improve upon the original calculations of Seljak (2000) and Scoccimarro et al. (2001) by taking into account the nonlinear evolution of matter clustering (Smith et al. 2003), halo exclusion, and the scaledependence of the halo bias factor…”
Accurate halo-model matter power spectra with dark energy, massive neutrinos and modified gravitational forces (2016, methodology): “We build on the work presented in Mead et al. (2015b) in which we developed a version of the standard halo model (Peacock & Smith 2000; Seljak 2000; Cooray & Sheth 2002) that produces matter power spectra that are accurate at the ' 5 per cent level for a range of standard cosmological parameters…”
Red Galaxy Growth and the Halo Occupation Distribution (2008, methodology): “Analytic methods of HOD modeling have been developed that allow quick computation of the galaxy space density and clustering statistics (HOD; e.g., Peacock & Smith 2000; Seljak 2000; Berlind & Weinberg 2002; Cooray & Sheth 2002).”
Towards a concordant model of halo occupation statistics (2006, background): “Early HOD models often assumed that 〈N〉M follows a simple power law (Jing, Mo & Börner 1998; Seljak 2000; Scoccimarro et al. 2001; Scranton 2002; Rozo, Dodelson & Frieman 2004; Collister & Lahav 2005) or a broken power law (Berlind & Weinberg 2002; Magliocchetti & Porciani 2003).”
The Coevolution of Galaxies and Supermassive Black Holes: Insights from Surveys of the Contemporary Universe (2014, background): “In the widely adopted halo-model description of large-scale structure, on small scales (< 1Mpc) the signal in the correlation function is dominated by pairs of galaxies within the same dark matter halo (known as the one-halo term; e.g. Seljak 2000).”
The 2dF Galaxy Redshift Survey: the dependence of galaxy clustering on luminosity and spectral type (2001, background): “The clustering pattern of galaxies is therefore determined by two processes: the spatial distribution of dark matter haloes and the manner in which dark matter haloes are populated by galaxies (Benson et al. 2000b; Peacock & Smith 2000; Seljak 2000; Berlind & Weinberg 2002).”
Formation of Galaxy Clusters (2012, background): “…if one assumes that all of the mass is in the collapsed halos, as is done for example in the halo models (Cooray & Sheth 2002), the requi ment that matter in the Universe is not biased against itself implies that ∫ b(ν)g(ν)d ln ν = 1 (e.g., Seljak 2000), whereg(ν) ≡ |d ln ν/d ln M|−1ψ(ν) (see eq.”
Baryonic Acoustic Oscillations in Simulated Galaxy Redshift Surveys (2005, methodology): “This holds even when the matter density field is nonlinear (Scherrer & Weinberg 1998; Coles et al. 1999; Seljak 2000).”
The 2dF Galaxy Redshift Survey: The bias of galaxies and the density of the Universe (2001, background): “Theoretical considerations suggest thatr ∼ 1 on scales of interest (e.g. Tegmark & Peebles 1998; Blanton et al. 2000; Seljak 2000).”
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 Dependence of Halo Clustering on Halo Formation History, Concentration, and Occupation (2005, methodology): “71 The second place these assumptions are commonly made is in the standard halo model of galaxy clustering (e.g., Seljak 2000; Peacock & Smith 2000; Scoccimarro et al. 2001; Berlind & Weinberg 2002; Bullock et al. 2002; Cooray & Sheth 2002).”
Inflation and the scale dependent spectral index: prospects and strategies (2010, background): “Non-linear biasing may be modeled via the halo occupation distribution (HOD) [68] or via higher order perturbation theory [69].”
The Shape of the Sloan Digital Sky Survey Data Release 5 Galaxy Power Spectrum (2007, background): “Seljak (2001) suggests that within the halo model (Seljak 2000; Peacock & Smith 2000; Cooray & Sheth 2002), there are two effects that may cause a scale-dependent bias for pairs of galaxies in different halos, which is particularly strong for LRGs (where the galaxies only occupy the most massive…”
Numerical simulations of the dark universe: State of the art and the next decade (2012, methodology): “which is normally taken from fitting formulae calibrated using predictions of DM simulations [232–236].”
COSMOLIKE - cosmological likelihood analyses for photometric galaxy surveys (2016, background): “…function, and the revised Halofit fitting formula of Takahashi et al. (2012) for non-linear evolution of the matter power spectrum or the halo model (Berlind & Weinberg 2002; Seljak 2000; Cooray et al. 2010) if one of the observables is not a linear projection of the matter density contrast.”
GALAXY CLUSTERING IN THE COMPLETED SDSS REDSHIFT SURVEY: THE DEPENDENCE ON COLOR AND LUMINOSITY (2010, methodology): “…through development of the Halo Occupation Distribution (HOD) framework (e.g., Jing, Mo, & Börner 1998; Ma & Fry 2000; Peacock & Smith 2000; Seljak 2000; Scoccimarro et al. 2001; Berlind & Weinberg 2002; Cooray & Sheth 2002; Yang, Mo, & van den Bosch 2003; Kravtsov et al. 2004; Zheng et…”
CARS: the CFHTLS-Archive-Research Survey - II. Weighing dark matter halos of Lyman-break galaxies at z = 3–5 (2009, background): “These deviations are explained by the halo model (see e.g. Seljak 2000; Cooray & Sheth 2002) as galaxy pairs in the same halo (one-halo term) allowing for a more accurate determination of the mean halo masses and also a measure of the mean number of galaxies hosted by a typical halo.”
The spatial and kinematic distributions of cluster galaxies in a ΩCDM universe: comparison with observations (2000, background): “In other words, we plot the evolution of the number of galaxies in a given magnitude interval per 1015M⊙ of cluster mass (assuming that the number of galaxies in the cluster scales roughly in proportion to its mass (see Seljak 2000, Sheth & Diaferio 2000)).”
The Halo Occupation Distribution: Toward an Empirical Determination of the Relation between Galaxies and Mass (2001, methodology): “Analytic Discussion Recent papers (Seljak 2000; Ma & Fry 2000; Scoccimarro et al. 2001; Sheth et al. 2001) present a fairly complete analytic theory of the galaxy correlation function in the halo bias model.”