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 - 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 -