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X-Ray Properties of SPT-selected Galaxy Clusters at 0.2
Name
Bulbul_2019_ApJ_871_50.pdf
Description
Published version
Size
3.67 MB
Format
Adobe PDF
Checksum (MD5)
8b35922aed246321fc843b6b10b5bccd
Author(s)
Bulbul, Esra
Chiu, I-Non
Mohr, Joseph J
McDonald, Michael
Benson, Bradford
Bautz, Mark W
Bayliss, Matthew
Bleem, Lindsey
Brodwin, Mark
Bocquet, Sebastian
Journal
Astrophysical Journal
Publisher
American Astronomical Society
Version
Final published version
Abstract
© 2019. The American Astronomical Society. All rights reserved. We present measurements of the X-ray observables of the intracluster medium (ICM), including luminosity L X , ICM mass M ICM , emission-weighted mean temperature T X , and integrated pressure Y X , that are derived from XMM-Newton X-ray observations of a Sunyaev-Zel'dovich effect (SZE) selected sample of 59 galaxy clusters from the South Pole Telescope SPT-SZ survey that span the redshift range 0.20 < z < 1.5. We constrain the best-fit power-law scaling relations between X-ray observables, redshift, and halo mass. The halo masses are estimated based on previously published SZE observable-to-mass scaling relations, calibrated using information that includes the halo mass function. Employing SZE-based masses in this sample enables us to constrain these scaling relations for massive galaxy clusters (M 500 ≥ 3 × 10 14 M o ) to the highest redshifts where these clusters exist without concern for X-ray selection biases. We find that the mass trends are steeper than self-similarity in all cases, and with ≥2.5σ significance in the case of L X and M ICM . The redshift trends are consistent with the self-similar expectation, but the uncertainties remain large. Core-included scaling relations tend to have steeper mass trends for L X . There is no convincing evidence for a redshift-dependent mass trend in any observable. The constraints on the amplitudes of the fitted scaling relations are currently limited by the systematic uncertainties on the SZE-based halo masses, but the redshift and mass trends are limited by the X-ray sample size and the measurement uncertainties of the X-ray observables.
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DOI of Published Version
10.3847/1538-4357/AAF230
