TY - JOUR
T1 - X-ray scaling relations from a complete sample of the richest maxBCG clusters
AU - Ge, Chong
AU - Sun, Ming
AU - Rozo, Eduardo
AU - Sehgal, Neelima
AU - Vikhlinin, Alexey
AU - Forman, William
AU - Jones, Christine
AU - Nagai, Daisuke
N1 - Funding Information:
We thank the referee, Gus Evrard, for important comments and suggestions. We thank Andrea Morandi for his early work on the Chandra data. Support for this work was provided by the National Aeronautics and Space Administration grants NNX16AH32G and NNX16AH26G. Support for this work was also provided by the National Aeronautics and Space Administration through Chandra Award Number GO4-15119B and GO4-15115X issued by the Chandra X-ray Center, which is operated by the Smithsonian Astrophysical Observatory for and on behalf of the National Aeronautics Space Administration under contract NAS8-03060. ER is supported by DOE grant DE-SC0015975 and by the Sloan Foundation grant FG-2016-6443. NS acknowledges support from NSF grant 1513618. DN acknowledges support from NSF grant AST-1412768. This research has made use of data and/or software provided by the High Energy Astrophysics Science Archive Research Center (HEASARC), which is a service of the Astrophysics Science Division at NASA/GSFC and the High Energy Astrophysics Division of the Smithsonian Astrophysical Observatory.
Publisher Copyright:
© 2019 The Author(s).
PY - 2019
Y1 - 2019
N2 - We 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 N200 ≥ 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|N), X = TX, LX, YX, to study the mass selection P(M|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 LX−TX and LX−YX 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.
AB - We 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 N200 ≥ 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|N), X = TX, LX, YX, to study the mass selection P(M|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 LX−TX and LX−YX 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.
KW - Galaxies: clusters: general
KW - Galaxies: clusters: intracluster medium
KW - X-rays: galaxies: clusters
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U2 - 10.1093/mnras/stz088
DO - 10.1093/mnras/stz088
M3 - Article
AN - SCOPUS:85063378783
SN - 0035-8711
VL - 484
SP - 1946
EP - 1971
JO - Monthly Notices of the Royal Astronomical Society
JF - Monthly Notices of the Royal Astronomical Society
IS - 2
ER -