CONSTRAINING THE SCATTER IN THE MASS–RICHNESS RELATION OF maxBCG CLUSTERS WITH WEAK LENSING AND X-RAY DATA

By E. Rozo, Eli S. Rykoff, August E. Evrard, M. Becker, T. McKay, Risa Wechsler, Benjamin P. Koester, Jiangang Hao, S. Hansen, Erin Sheldon and 3 more. 2008

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We measure the logarithmic scatter in mass at fixed richness for clusters in the maxBCG cluster catalog, an optically selected cluster sample drawn from Sloan Digital Sky Survey imaging data. Our measurement is achieved by demanding consistency between available weak-lensing and X-ray measurements of the maxBCG clusters, and the X-ray luminosity–mass relation inferred from the 400 days X-ray cluster survey, a flux-limited X-ray cluster survey. We find (95% CL) at N200 ≈ 40, where N200 is the number of red sequence galaxies in a cluster. As a byproduct of our analysis, we also obtain a constraint on the correlation coefficient between ln LX and ln M at fixed richness, which is best expressed as a lower limit, rL,M|N ⩾ 0.85(95% CL). This is the first observational constraint placed on a correlation coefficient involving two different cluster mass tracers. We use our results to produce a state-of-the-art estimate of the halo mass function at z = 0.23—the median redshift of the maxBCG cluster sample—and find that it is consistent with the WMAP5 cosmology. Both the mass function data and its covariance matrix are presented.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/d1ecf0a687e75ad9081375b2b4271f32c3435836

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Citations in the corpus

DARK MATTER HALOS IN THE STANDARD COSMOLOGICAL MODEL: RESULTS FROM THE BOLSHOI SIMULATION (2010, result): “The Bolshoi parameters are in excellent agreement with the SDSS maxBCG+WMAP5 cosmological parameters (Rozo et al. 2009).”
Planck2013 results. XXIX. ThePlanckcatalogue of Sunyaev-Zeldovich sources (2013, methodology): “We define a quality criterion for the association,QSDSS, in terms of cluster richness as a proxy of the cluster mass (see for instanceJohnston et al. 2007; Rozo et al. 2009).”
Weak Lensing Measurement of the Mass--Richness Relation of SDSS redMaPPer Clusters (2016, methodology): “redMaPPer is a red-sequence photometric cluster finding algorithm (Rykoff et al. 2014, hereafter RM I), built around the optimized richness estimator developed in Rozo et al. (2009b) and Rykoff et al. (2012).”
A WEAK LENSING STUDY OF X-RAY GROUPS IN THE COSMOS SURVEY: FORM AND EVOLUTION OF THE MASS–LUMINOSITY RELATION (2009, background): “…it is sensitive to both the expansion and growth history of the universe and can be used to constrain cosmological parameters such as Ωm, σ8, and ΩΛ (e.g. White et al. 1993; Wang & Steinhardt 1998; Haiman et al. 2001; Rozo et al. 2004; Wang et al. 2004a; Bahcall et al. 2004; Rozo et al. 2009).”
The relation between velocity dispersion and mass in simulated clusters of galaxies: dependence on the tracer and the baryonic physics (2013, background): “…(e.g. Arnaud et al. 2010; Williamson et al. 2011; Kay et al. 2012) observations, the optical luminosity or richness traced by the cluster galaxy population (e.g. Popesso et al. 2007; Rozo et al. 2009), and velocity dispersion of member galaxies (e.g. Biviano et al. 2006; Saro et al. 2012).”
Galactic accretion and the outer structure of galaxies in the CDM model (2013, background): “Some of this disagreement may be due to a mismatch in the averageM200 of the galaxies being compared, as mass–richness relations suggest that the typical halo mass of the Zibetti et al. sample is M200 & 1014.2 M (e.g. Rozo et al. 2009).”
Cosmological Parameters from Observations of Galaxy Clusters (2011, background): “To date, the only empirical estimates of such correlation are for mass and X-ray luminosity at fixed optical richness, r(LX,M |Ngal) ≥ 0.85 (Rozo et al. 2009); and for soft-band X-ray luminosity and temperature at fixed mass, r(LX, TX|M) = 0.09 ± 0.19 (Mantz et al. 2010a).”
A CATALOG OF 132,684 CLUSTERS OF GALAXIES IDENTIFIED FROM SLOAN DIGITAL SKY SURVEY III (2012, background): “The scatter in mass based on our richness is also in agreement with that based on the maxBCG richness (Rozo et al. 2009a).”
ROBUST OPTICAL RICHNESS ESTIMATION WITH REDUCED SCATTER (2011, methodology): “…catalog (Koester et al. 2007a), which is currently the beststudied optically selected cluster catalog at moderate redshifts 17 As discussed in Rozo et al. (2009b), throughout this work the word “richness” is meant to be understood as “optical mass tracer,” and is not necessarily the actual…”
Scaling relations for galaxy clusters in the Millennium-XXL simulation (2012, methodology): “…route (Nopt → M500 → YSZ) using the mean weak lensing masses measured as a function of Nopt for stacked maxBCG clusters by Johnston et al. (2007) and Rozo et al. (2009) who in addition corrected Mlens upwards to account for an improved model for the redshift distribution of the source galaxy…”
The BAHAMAS project: Calibrated hydrodynamical simulations for large-scale structure cosmology (2016, methodology): “Specifically, Becker et al. (2007) derive the mean of the log of the velocity dispersion in richness bins; i.e., 〈log σgal,1D〉 (N), while Rozo et al. (2009) derive the mean halo mass in richness bins; i.e., 〈M500,c〉 (N) (see Appendix A of Rozo et al.).”
Towards a realistic population of simulated galaxy groups and clusters (2013, methodology): “…panel) has a significantly higher mean luminosity than the Osmond & Ponman (2004) X-ray-selected sample (black semi-circles in the left panel), the Rozo et al. (2009) optically-selected sample (black lines in the right panel), and the Leauthaud et al. (2010) Xray-selected sample (black squares in…”
GALAXIES IN ΛCDM WITH HALO ABUNDANCE MATCHING: LUMINOSITY–VELOCITY RELATION, BARYONIC MASS–VELOCITY RELATION, VELOCITY FUNCTION, AND CLUSTERING (2010, result): “The Bolshoi parameters are in excellent agreement with the SDSS maxBCG+WMAP5 cos mological parameters (Rozo et al. 2009) and with cosmological parameters from WMAP5 plus recent X-ray cluster survey re sults (Klypin et al. 2010).”