On the Mass-to-Light Ratio of Large-Scale Structure

By J. Tinker, D. Weinberg, Zheng Zheng, Idit Zehavi. 2004

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We examine the dependence of the mass-to-light (M/L) ratio of large-scale structure on cosmological parameters, in models that are constrained to match observations of the projected galaxy correlation function wp(rp) and the galaxy luminosity function. For a sequence of cosmological models with a fixed, observationally motivated power spectrum shape and increasing normalization σ8, we find parameters of the galaxy halo occupation distribution (HOD) that reproduce wp(rp) measurements as a function of luminosity from the Sloan Digital Sky Survey (SDSS). From these HOD models we calculate the r-band conditional luminosity function Φ(L|Mh), and from this the mean M/L ratio as a function of halo mass Mh. We also use Φ(L|Mh) to populate halos of N-body simulations with galaxies and thereby compute M/L in a range of large-scale environments, including cluster infall regions. For all cosmological models, the M/L ratio in high-mass halos or high-density regions is approximately independent of halo mass or smoothing scale. However, the "plateau" value of M/L depends on σ8 in addition to the obvious proportionality with the matter density parameter Ωm, and it represents the universal value ⟨M/L⟩ = Ωmρcrit/ρlum only for models in which the galaxy correlation function is approximately unbiased, i.e., with σ8 ≈ σ8g. Our results for cluster mass halos follow the trend (M/L)cl = 577(Ωm/0.3)(σ8/0.9)1.7 h M☉/L☉. Combined with the mean M/L ratio for CNOC galaxy clusters, this relation implies (σ8/0.9)(Ωm/0.3)0.6 = 0.75 ± 0.06. M/L estimates for SDSS clusters and the virial regions of clusters in the CAIRNS survey imply a similar value of σ8Ω, while the CAIRNS estimates for cluster infall regions imply a lower value. These results are inconsistent with parameter values Ωm ≈ 0.3, σ8 ≈ 0.9 favored by recent joint analyses of cosmic microwave background measurements and other large-scale structure data, although they agree with values inferred from the van den Bosch et al. analysis of the 2dF Galaxy Redshift Survey. We discuss possible resolutions of this discrepancy, none of which seems entirely satisfactory. In appendices we present an improved formula for halo bias factors calibrated on our 3603 N-body simulations and an improved analytic technique for calculating the galaxy correlation function from a given cosmological model and HOD.

Subfields: Astronomy and Astrophysics, Ecology, Instrumentation

View Paper: https://www.semanticscholar.org/paper/b15241f7eafb79b045154118f6c82f3e4edea10a

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Citations in the corpus

CFHTLenS: the relation between galaxy dark matter haloes and baryons from weak gravitational lensing (2013, methodology): “We also assume that the dependence of the galaxy bias on mass follows the prescription from Sheth et al. (2001), incorporating the adjustments described in Tinker et al. (2005).”
THE GALAXY CONTENT OF SDSS CLUSTERS AND GROUPS (2007, background): “The (M/L)200–M200 relationship is both expected theoretically in some models (e.g., Tinker et al. 2005; van den Bosch et al. 2007, and references therein) and directly observed (Sheldon et al. 2007b).”
Ray-tracing through the Millennium Simulation: Born corrections and lens-lens coupling in cosmic shear and galaxy-galaxy lensing (2008, background): “This coincides with the transition region of the one- and two-halo terms, which is difficult to model accurately due to halo exclusion effects (see e.g. Tinker et al. 2005, and references therein), which are not included in our prediction.”
Towards a concordant model of halo occupation statistics (2006, background): “…is the critical overdensity required for spherical collapse at redshift z, and σ (M) is the linear theory rms mass fluctuation on the mass scale M. Tinker et al. (2005), using state-of-the-art numerical simulations, reinvestigated the mass dependence of the halo bias, and found that equation…”
Cosmological constraints from a combination of galaxy clustering and lensing – I. Theoretical framework (2012, methodology): “…methods that have been advocated and which typically involve adopting an upper limit for the mass interval used in the integral for the 2-halo term of the power spectrum (e.g., Takada & Jain 2003; Zheng 2004; Abazajian et al. 2005; Tinker et al. 2005, 2012; Yoo et al. 2006; Leauthaud et al. 2011).”
He ii REIONIZATION AND ITS EFFECT ON THE INTERGALACTIC MEDIUM (2008, background): “…relationship to relate a galaxy’s stellar mass to its super-massive black hole mass (Hopkins et al. 2007a,b), and the halo occupation model of Tinker et al. (2005); Conroy et al. (2006); Vale & Ostriker (2006) (for details, see Hopkins et al. (2008a)) to map from halo mass to stellar…”
Cosmological Constraints from a Combination of Galaxy Clustering and Lensing -- III. Application to SDSS Data (2012, methodology): “As described in Appendix A, the scale dependence of the halo bias in the quasi-linear regime is described by a modified version of the empirical fitting function of Tinker et al. (2005).”
HALO OCCUPATION DISTRIBUTION MODELING OF CLUSTERING OF LUMINOUS RED GALAXIES (2008, methodology): “We essentially follow the method presented in Zehavi et al. (2005b) and adopt the improvements of Tinker et al. (2005) for theoretical modeling of the two-point auto- and crosscorrelation functions in the HOD framework.”
A COMPREHENSIVE ANALYSIS OF UNCERTAINTIES AFFECTING THE STELLAR MASS–HALO MASS RELATION FOR 0 < z < 4 (2010, background): “Halo occupation (e.g., Berlind & Weinberg 2002; Bullock et al. 2002; Cooray & Sheth 2002; Tinker et al. 2005; Zheng et al. 2007) and conditional luminosity function modeling (e.g., Yang et al. 2003; Cooray 2006) fall into this category.”
Halo mass function and scale-dependent bias from N-body simulations with non-Gaussian initial conditions (2008, methodology): “Our results are in good agreement with the fit by Sheth et al. (2001) for large masses and with that by Tinker et al. (2005) for smaller 2 Consistently, in what follows, we use the rms value as the error on b(k, M , z, f NL = 0).”
MERGERS IN ΛCDM: UNCERTAINTIES IN THEORETICAL PREDICTIONS AND INTERPRETATIONS OF THE MERGER RATE (2010, methodology): “In the former, one paints galaxies onto host halos with no regard for halo merger histories or dark mattersubstructure, using clustering as a constraint (see e.g. Yan et al. 2003; Yang et al. 2003; Tinker et al. 2005; Kravtsov et al. 2004; Wechsler et al. 2006).”
Galactic star formation and accretion histories from matching galaxies to dark matter haloes (2012, background): “…or type) within main haloes of a given mass is constrained using galaxy abundance and clustering statistics (e.g. Peacock & Smith 2000; White 2001; Berlind & Weinberg 2002; Zehavi et al. 2004; Tinker et al. 2005; Brown et al. 2008; Zehavi et al. 2011; Wake et al. 2011; Leauthaud et al. 2012).”
hmcode-2020: improved modelling of non-linear cosmological power spectra with baryonic feedback (2020, methodology): “With reasonable choices, the model has been shown to be accurate for the matter–matter power spectrum at only the∼ 30 per-cent level compared to accurate spectra measured from simulations (e.g., Tinker et al. 2005; Valageas & Nishimichi 2011; Mead et al. 2015).”
Theoretical Models of the Halo Occupation Distribution: Separating Central and Satellite Galaxies (2004, result): “Tinker et al. (2005) show that the SDSS correlation function constraints and observational estimates of cluster mass-to-light ratios imply that the values of Ωm and/or σ8 are lower than the traditionally adopted “concordance” values of 0.3 and 0.9, in agreement with van den Bosch, Mo, & Yang’s…”
The Dependence of Halo Clustering on Halo Formation History, Concentration, and Occupation (2005, background): “Abbas & Sheth (2006) showed that the observed environmental dependence of clustering in SDSS could be fully accounted for by correlations between galaxy properties and host mass and by correlations between host mass and environment.”
CIRS: Cluster Infall Regions in the Sloan Digital Sky Survey. I. Infall Patterns and Mass Profiles (2006, background): “…prediction for the dependence of mass-to-light ratio on halo mass. Comparing their simulations to observed mass-to-light ratios of cluster virial regions, Tinker et al. (2005) concluded that models with values of σ8 and/or Ωm smaller than those found by Tegmark et al. (2004) provide the best fits.”