X-ray scaling relations from a complete sample of the richest maxBCG clusters
AffiliationUniv Arizona, Dept Phys
Keywordsgalaxies: clusters: general
galaxies: clusters: intracluster medium
X-rays: galaxies: clusters
MetadataShow full item record
PublisherOXFORD UNIV PRESS
CitationChong Ge, Ming Sun, Eduardo Rozo, Neelima Sehgal, Alexey Vikhlinin, William Forman, Christine Jones, Daisuke Nagai, X-ray scaling relations from a complete sample of the richest maxBCG clusters, Monthly Notices of the Royal Astronomical Society, Volume 484, Issue 2, April 2019, Pages 1946–1971, https://doi.org/10.1093/mnras/stz088
Rights© 2019 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society
Collection InformationThis item from the UA Faculty Publications collection is made available by the University of Arizona with support from the University of Arizona Libraries. If you have questions, please contact us at firstname.lastname@example.org.
AbstractWe use a complete sample of 38 richest maxBCG clusters to study the ICM-galaxy scaling relations and the halo mass selection properties of the maxBCG algorithm, based on X-ray and optical observations. The clusters are selected from the two largest bins of optical richness in the Planck stacking work with the maxBCG richness N-200 >= 78. We analyse their Chandra and XMM Newton data to derive the X-ray properties of the ICM. We then use the distribution of P(X vertical bar N), X = T-X, L-X, Y-X, to study the mass selection P(M vertical bar N) of maxBCG. Compared with previous works based on the whole richness sample, a significant fraction of blended systems with boosted richness is skewed into this richest sample. Parts of the blended haloes are picked apart by the redMaPPer, an updated red-sequence cluster finding algorithm with lower mass scatter. Moreover, all the optical blended haloes are resolved as individual X-ray haloes, following the established L-X-T-X and L-X-Y-X relations. We further discuss that the discrepancy between ICM-galaxy scaling relations, especially for future blind stacking, can come from several factors, including miscentring, projection, contamination of low-mass systems, mass bias, and covariance bias. We also evaluate the fractions of relaxed and cool core clusters in our sample. Both are smaller than those from SZ or X-ray selected samples. Moreover, disturbed clusters show a higher level of mass bias than relaxed clusters.
VersionFinal published version
SponsorsNational Aeronautics and Space Administration [NNX16AH32G, NNX16AH26G]; National Aeronautics and Space Administration through Chandra Award [GO4-15119B, GO4-15115X]; National Aeronautics Space Administration [NAS8-03060]; DOE [DE-SC0015975]; Sloan Foundation [FG-2016-6443]; NSF [AST-1412768, 1513618]