Cross-correlation Weak Lensing of SDSS Galaxy Clusters I: Measurements

Sheldon, Erin S. ; Johnston, David E. ; Scranton, Ryan ; Koester, Ben P. ; McKay, Timothy A. ; Oyaizu, Hiroaki ; Cunha, Carlos ; Lima, Marcos ; Lin, Huan ; Frieman, Joshua A. ; Wechsler, Risa H. ; Annis, James ; Mandelbaum, Rachel ; Bahcall, Neta A. ; Fukugita, Masatak

关键词: GALAXIES;    GALAXY CLUSTERS;    LUMINOSITY;    SKY Astrophysics;    ASTRO;   

DOI  :  10.2172/917269
RP-ID  :  SLAC-PUB-12811
PID  :  OSTI ID: 917269
Others  :  Other: arXiv:0709.1153
Others  :  TRN: US200816%%467

学科分类：物理（综合）

美国|英语

来源: SciTech Connect

【 摘 要 】

This is the first in a series of papers on the weak lensing effect caused by clusters of galaxies in Sloan Digital Sky Survey. The photometrically selected cluster sample, known as MaxBCG, includes {approx}130,000 objects between redshift 0.1 and 0.3, ranging in size from small groups to massive clusters. We split the clusters into bins of richness and luminosity and stack the surface density contrast to produce mean radial profiles. The mean profiles are detected over a range of scales, from the inner halo (25 kpc/h) well into the surrounding large scale structure (30 Mpc/h), with a significance of 15 to 20 in each bin. The signal over this large range of scales is best interpreted in terms of the cluster-mass cross-correlation function. We pay careful attention to sources of systematic error, correcting for them where possible and bounding them where not. We find that the profiles scale strongly with richness and luminosity. We find the signal within a given richness bin depends upon luminosity, suggesting that luminosity is more closely correlated with mass than galaxy counts. We split the samples by redshift but detect no significant evolution. The profiles are not well described by power laws. In a subsequent series of papers we invert the profiles to three-dimensional mass profiles, show that they are well fit by a halo model description, measure mass-to-light ratios and provide a cosmological interpretation.