Baryon content of massive galaxy clusters at 0.57
Name
1412.7823.pdf
Description
Accepted version
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765.07 KB
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Author(s)
Chiu, I
Mohr, J
McDonald, M
Bocquet, S
Ashby, MLN
Bayliss, M
Benson, BA
Bleem, LE
Brodwin, M
Desai, S
Date Issued
2016
Journal
Monthly Notices of the Royal Astronomical Society
Publisher
Oxford University Press (OUP)
Citation
Chiu, I., et al. "Baryon Content of Massive Galaxy Clusters at 0.57 < Z < 1.33." Monthly Notices of the Royal Astronomical Society 455 1 (2016): 258-75.
Version
Author's final manuscript
Abstract
© 2015 The Authors. We study the stellar, brightest cluster galaxy (BCG) and intracluster medium (ICM) masses of 14 South Pole Telescope (SPT) selected galaxy clusters with median redshift z = 0.9 and mass M500 = 6 × 1014M⊙. We estimate stellar masses for each cluster and BCG using six photometric bands, the ICM mass using X-ray observations and the virial masses using the SPT Sunyaev-Zel'dovich effect signature. At z = 0.9, the BCG mass M*BCG constitutes 0.12 ± 0.01 per cent of the halo mass for a 6 × 1014M⊙ cluster, and this fraction falls as M 500-0.58±0.07. The cluster stellar mass function has a characteristic mass M0 = 1011.0 ± 0.1M⊙, and the number of galaxies per unit mass in clusters is larger than in the field by a factor of 1.65 ± 0.20. We combine our SPT sample with previously published samples at low redshift and correct to a common initial mass function and for systematic virial mass differences. We then explore mass and redshift trends in the stellar fraction f*, the ICM fraction fICM, the collapsed baryon fraction fc and the baryon fraction fb. At a pivot mass of 6 × 1014M⊙ and redshift z = 0.9, the characteristic values are f* = 1.1 ± 0.1 per cent, fICM = 9.6 ± 0.5 per cent, fc = 10.7 ± 1.1 per cent and fb = 10.7 ± 0.6 per cent. These fractions all vary with cluster mass at high significance, with higher mass clusters having lower f* and fc and higher fICM and fb. When accounting for a 15 per cent systematic virial mass uncertainty, there is no statistically significant redshift trend at fixed mass. Our results support the scenario where clusters grow through accretion from subclusters (higher f*, lower fICM) and the field (lower f*, higher fICM), balancing to keep f* and fICM approximately constant since z ~ 0.9.
MIT Department
MIT Kavli Institute for Astrophysics and Space Research
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DOI of Published Version
https://doi.org/10.1093/MNRAS/STV2303
