Cross-correlation Weak Lensing of SDSS galaxy Clusters II: Cluster Density Profiles and the Mass--Richness Relation

By D. Johnston, Erin Sheldon, Risa Wechsler, E. Rozo, Benjamin P. Koester, Joshua A. Frieman, T. McKay, August E. Evrard, Matthew R. Becker, James Annis. 2007

181 citations recorded by the source corpus.

We interpret and model the statistical weak lensing measurements around 130,000 groups and clusters of galaxies in the Sloan Digital Sky Survey presented by Sheldon et al. (2007). We present non-parametric inversions of the 2D shear profiles to the mean 3D cluster density and mass profiles in bins of both optical richness and cluster i-band luminosity. Since the mean cluster density profile is proportional to the cluster-mass correlation function, the mean profile is spherically symmetric by the assumptions of large-scale homogeneity and isotropy. We correct the inferred 3D profiles for systematic effects, including non-linear shear and the fact that cluster halos are not all precisely centered on their brightest galaxies. We also model the measured cluster shear profile as a sum of contributions from the brightest central galaxy, the cluster dark matter halo, and neighboring halos. We infer the relations between mean cluster virial mass and optical richness and luminosity over two orders of magnitude in cluster mass; the virial mass at fixed richness or luminosity is determined with a precision of {approx} 13% including both statistical and systematic errors. We also constrain the halo concentration parameter and halo bias as a function of cluster mass; both are in good agreement with predictions from N-body simulations of LCDM models. The methods employed here will be applicable to deeper, wide-area optical surveys that aim to constrain the nature of the dark energy, such as the Dark Energy Survey, the Large Synoptic Survey Telescope and space-based surveys.

Subfields: Astronomy and Astrophysics, Atomic and Molecular Physics, and Optics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/53edf42558acb5a6937057a30cbdcbcc2b94904e

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Citations in the corpus

CLASH: JOINT ANALYSIS OF STRONG-LENSING, WEAK-LENSING SHEAR, AND MAGNIFICATION DATA FOR 20 GALAXY CLUSTERS (2015, background): “…physical length units (Okabe et al. 2010, 2013; Umetsu et al. 2011a, 2014), which makes the effective halo mass extracted from the averaged lensing signal a good proxy for the mean population value (see Section 5.4; Johnston et al. 2007; Okabe et al. 2013; Umetsu et al. 2014; Sereno et al. 2015c).”
Planck2013 results. XXIX. ThePlanckcatalogue of Sunyaev-Zeldovich sources (2013, background): “It has proven difficult to capitalize on the large size of optical/IR cluster samples because the observable, the number of galaxies in each cluster, exhibits large scatter with respect to the total cluster mass (e.g.,Johnston et al. 2007).”
LoCuSS: Subaru Weak Lensing Study of 30 Galaxy Clusters (2009, background): “…around clusters binned on cluster richness, X-ray luminosity, etc. — the so-called stacked lens (Mandelbaum et al. 2008; Sheldon et al. 2009a, 2009b; Johnston et al. 2007), where the average properties of cluster mass profiles as well as the average mass-observable relation can be obtained, but…”
Weighing the Giants - I. Weak-lensing masses for 51 massive galaxy clusters: project overview, data analysis methods and cluster images (2012, background): “For larger samples of less massive systems, stacking analyses enable the determination of the mean cluster mass in bins of survey observable (Johnston et al. 2007; Leauthaud et al. 2010).”
Observational probes of cosmic acceleration (2012, background): “Mis-centering is currently one of the dominant systematics in stacked cluster lensing, introducing uncertainties at the ≈ 5% − 10% level (Johnston et al., 2007).”
Detailed cluster lensing profiles at large radii and the impact on cluster weak lensing studies (2011, methodology): “…lensing technique has been applied to the Sloan Digital Sky Survey data to obtain constraints on cosmological parameters (Mandelbaum & Seljak 2007; Johnston et al. 2007; Sheldon et al. 2009; Rozo et al. 2010), and will offer a promising mass-calibration method in future wide-field optical imaging…”
Dark Energy Survey Year 1 results: weak lensing mass calibration of redMaPPer galaxy clusters (2018, background): “When a cluster is miscentred by some radial offset Rmis, the corresponding azimuthally averaged surface mass density is (e.g. Yang et al. 2006; Johnston et al. 2007) mis(R | Rmis) = ∫ 2π 0 dθ 2π (√ R2 + R2mis − 2RRmis cos θ ) .”
Are Brightest Halo Galaxies Central Galaxies (2010, background): “…such as satellite kinematics (e.g., McKay et al. 2002; van den Bosch et al. 2004; More et al. 2009), weak lensing (e.g., Mandelbaum et al. 2006; Johnston et al. 2007; Cacciato et al. 2009; Sheldon et al. 2009b), and strong lensing (e.g., Kochanek 1995; Cohn et al. 2001; Koopmans & Treu 2003;…”
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): “…Brainerd et al. 1996; McKay et al. 2001; Hoekstra et al. 2004; Sheldon et al. 2004, 2009; Mandelbaum et al. 2006a, 2006b; Heymans et al. 2006a; Johnston et al. 2007; Leauthaud et al. 2010) and the kinematics of satellite galaxies (McKay et al. 2002; Prada et al. 2003; Brainerd & Specian…”
Combined strong and weak lensing analysis of 28 clusters from the Sloan Giant Arcs Survey (2011, methodology): “This stacked lensing analysis has c© RAS, MNRAS 000, 1–22 been successful for constraining mean dark matter distributions of cluster samples (e.g., Mandelbaum et al. 2006b; Johnston et al. 2007; Leauthaud et al. 2010; Okabe et al. 2010).”
THE GALAXY CONTENT OF SDSS CLUSTERS AND GROUPS (2007, methodology): “We apply the nonparametric method of Johnston et al. (2007a) to deproject the number density profiles.”
Weak Lensing Measurement of the Mass--Richness Relation of SDSS redMaPPer Clusters (2016, methodology): “Our peak value is smaller than the simulations of the MaxBCG cluster sample (Johnston et al. 2007a) of ∼ 0.4h−1 Mpc, although as that catalogue uses different methods of finding the centre of a galaxy clusters, discrepancies should be expected.”
CLASH: WEAK-LENSING SHEAR-AND-MAGNIFICATION ANALYSIS OF 20 GALAXY CLUSTERS (2014, background): “Johnston et al. (2007) demonstrated that the smoothing effects of miscentering on ∆Σ+ are much larger than on Σ, and produce a noticeable effect on ∆Σ+ out to 10 times the typical positional offset from the cluster mass centroid (Johnston et al. 2007).”
Cosmological Parameters from Observations of Galaxy Clusters (2011, methodology): “Stacking analyses of clusters detected in survey fields have also proved successful in calibrating the mean mass–observable scaling relations down to relatively low masses (e.g. Johnston et al. 2007; Rykoff et al. 2008; Leauthaud et al. 2010).”