Galaxy clustering and galaxy-galaxy lensing: a promising union to constrain cosmological parameters

By M. Cacciato, F. V. D. Bosch, S. More, Ran Li, H. Mo, Xiaohu Yang. 2008

139 citations recorded by the source corpus.

Galaxy clustering and galaxy-galaxy lensing probe the connection between galaxies and their dark matter haloes in complementary ways. Since the clustering of dark matter haloes depends on cosmology, the halo occupation statistics inferred from the observed clustering properties of galaxies are degenerate with the adopted cosmology. Consequently, different cosmologies imply different mass-to-light ratios for dark matter haloes. Galaxy-galaxy lensing, which yields direct constraints on the actual mass-to-light ratios, can therefore be used to break this degeneracy, and thus to constrain cosmological parameters. In this paper, we establish the link between galaxy luminosity and dark matter halo mass using the conditional luminosity function (CLF), Phi(L\M) dL, which gives the number of galaxies with luminosities in the range L +/- dL/2 that reside in a halo of mass M. We constrain the CLF parameters using the galaxy luminosity function and the luminosity dependence of the correlation lengths of galaxies. The resulting CLF models are used to predict the galaxy-galaxy lensing signal. For a cosmology that agrees with constraints from the cosmic microwave background, i.e. (Omega(m), sigma(8)) = (0.238, 0.734), the model accurately fits the galaxy-galaxy lensing data obtained from the Sloan Digital Sky Survey. For a comparison cosmology with (Omega(m), sigma(8)) = (0.3, 0.9), however, we can accurately fit the luminosity function and clustering properties of the galaxy population, but the model predicts mass-to-light ratios that are too high, resulting in a strong overprediction of the galaxy-galaxy lensing signal. We conclude that the combination of galaxy clustering and galaxy-galaxy lensing is a powerful probe of the galaxy-dark matter connection, with the potential to yield tight constraints on cosmological parameters. Since this method mainly probes the mass distribution on relatively small (non-linear) scales, it is complementary to constraints obtained from the galaxy power spectrum, which mainly probes the large-scale (linear) matter distribution.

Subfields: Astronomy and Astrophysics, Electrical and Electronic Engineering, Global and Planetary Change

View Paper: https://www.semanticscholar.org/paper/3ac6e7f6172d80fa919f971ba93b936228268295

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Citations in the corpus

THE CONNECTION BETWEEN GALAXIES AND DARK MATTER STRUCTURES IN THE LOCAL UNIVERSE (2012, methodology): “…related to cosmological parameters — and the galaxies that trace it is likely to be a dominant systematic in studies of cosmic acceleration with galaxy surveys using a range of probes (e.g., Cacciato et al. 2009; More et al. 2009; Tinker et al. 2011; Nuza et al. 2012 and references therein).”
Cosmological constraints from a combination of galaxy clustering and lensing – I. Theoretical framework (2012, methodology): “In the lower panels we use the WMAP3 cosmology, i.e., the cosmological parameters that best fit the three year data release of the Wilkinson Microwave Anisotropy Probe (Spergel et al. 2007) and the best-fit CLF model for that cosmology obtained by Cacciato et al. (2009).”
The stellar mass-halo mass relation of isolated field dwarfs : a critical test of ΛCDM at the edge of galaxy formation (2016, background): “However, most studies to date have focussed on the high mass end of this relation where the differences between ΛCDM and alternative cosmologies like Λ Warm Dark Matter (ΛWDM) are small (e.g. Cacciato et al. 2009; Shan et al. 2015; and see Figure 3).”
The kinematic connection between galaxies and dark matter haloes (2010, background): “…lensing (e.g., Brainerd et al. 1996; Hudson et al. 1998; Wilson et al. 2001; Guzik & Seljak 2002; Hoekstra, Yee & Gladders 2004; Mandelbaum et al. 2006; Cacciato et al. 2009) and satellite kinematics (e.g., Zaritsky & White 1994; Prada et al. 2003; van den Bosch et al. 2004; Conroy et al. 2005).”
Cosmological parameter constraints from galaxy-galaxy lensing and galaxy clustering with the SDSS DR7 (2012, methodology): “Alternative approaches involving halo occupation distribution (HOD) modeling have also been considered (Yoo et al. 2006; Cacciato et al. 2009; Leauthaud et al. 2011; Cacciato et al. 2012a; Leauthaud et al. 2012; Tinker et al. 2012; van den Bosch et al. 2012) as ways to combine the galaxy-galaxy…”
THE PSEUDO-EVOLUTION OF HALO MASS (2012, background): “…Zehavi et al. 2005; Skibba et al. 2006; van den Bosch et al. 2007; Brown et al. 2008; Conroy & Wechsler 2009; Moster et al. 2010, 2013; Behroozi et al. 2010; Yang et al. 2012), or a combination of the above probes (Yoo et al. 2006; Cacciato et al. 2009; Leauthaud et al. 2012; More et al. 2012).”
GALAXY CLUSTERING IN THE COMPLETED SDSS REDSHIFT SURVEY: THE DEPENDENCE ON COLOR AND LUMINOSITY (2010, methodology): “A number of papers have implemented variants of this approach to constrain the matter density parameter Ωm and the amplitude of matter clustering σ8 (van den Bosch, Mo, & Yang 2003b; Abazajian et al. 2005; Tinker et al. 2005; van den Bosch et al. 2007; Cacciato et al. 2009; Rozo et al. 2010).”
Detailed cluster lensing profiles at large radii and the impact on cluster weak lensing studies (2011, background): “Indeed, earlier work using N-body simulations has found the significant contribution of correlated matter around haloes (e.g., Mandelbaum et al. 2005; Hayashi & White 2008; Tavio et al. 2008; Cacciato et al. 2009; Hilbert & White 2010; Masaki 2011).”
Cosmological Constraints from a Combination of Galaxy Clustering and Lensing -- III. Application to SDSS Data (2012, methodology): “Examples are the 1-halo to 2-halo transition (e.g., Zehavi et al. 2004) and the 1-halo central to 1-halo satellite transition for the excess surface densities (e.g., Cacciato et al. 2009).”
Dependence of galaxy quenching on halo mass and distance from its centre (2012, background): “For central galaxies, it has been established with high confidence (e.g., Cacciato et al. 2009; More et al. 2009; Mandelbaum et al. 2009; Leauthaud et al. 2011, 2012) that the relation with the halo mass is somewhat steeper at low mass than at high mass.”
Satellite kinematics – III. Halo masses of central galaxies in SDSS (2010, unknown): “Yang et al. (2007) studied galaxy groups in the SDSS, which they assigned halo masses based upon either the total stellar mass or the total luminosity content of each group.”
Simultaneous measurement of cosmology and intrinsic alignments using joint cosmic shear and galaxy number density correlations (2009, background): “…al. 2007; Padmanabhan et al. 2007) galaxygalaxy lensing (e.g. Schneider & Rix 1997; Guzik & Seljak 2001, 2002; Seljak 2002; Seljak et al. 2005; Yoo et al. 2006; Johnston et al. 2007; Cacciato et al. 2009) and lensing magnification (Broadhurst et al. 1995; Zhang & Pen 2005, 2006; van Waerbeke 2010).”