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Title: X-Ray Properties of SPT Selected Galaxy Clusters at 0.2<z<1.5 Observed with XMM-Newton

Abstract

We present measurements of the X-ray observables of the intra-cluster 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 ($$M_{500}\geq 3 \times10^{14}$$ $$M_\odot$$) 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 $$\geq 2.5{\sigma}$$ significance in the case of $$L_X$$ and $$M_{ICM}$$. The redshift trends are consistent with the self-similar expectation in all cases, 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 log-normal intrinsic scatter in the observable at fixed halo mass varies from $$\sim$$0.10 for $$M_{ICM}$$ and core-excised $$Y_X$$ to $$\sim$$0.27 for core-included bolometric $$L_X$$. 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 (abridged).

Authors:
Publication Date:
Research Org.:
Argonne National Lab. (ANL), Argonne, IL (United States); Fermi National Accelerator Lab. (FNAL), Batavia, IL (United States)
Sponsoring Org.:
USDOE Office of Science (SC), High Energy Physics (HEP) (SC-25)
Contributing Org.:
SPT
OSTI Identifier:
1468410
Report Number(s):
FERMILAB-PUB-18-319-AE; arXiv:1807.02556
1681485
DOE Contract Number:  
AC02-07CH11359
Resource Type:
Journal Article
Journal Name:
Astrophys.J.
Additional Journal Information:
Journal Name: Astrophys.J.
Country of Publication:
United States
Language:
English
Subject:
79 ASTRONOMY AND ASTROPHYSICS

Citation Formats

Bulbul, Esra, and et al. X-Ray Properties of SPT Selected Galaxy Clusters at 0.2<z<1.5 Observed with XMM-Newton. United States: N. p., 2018. Web.
Bulbul, Esra, & et al. X-Ray Properties of SPT Selected Galaxy Clusters at 0.2<z<1.5 Observed with XMM-Newton. United States.
Bulbul, Esra, and et al. Fri . "X-Ray Properties of SPT Selected Galaxy Clusters at 0.2<z<1.5 Observed with XMM-Newton". United States. https://www.osti.gov/servlets/purl/1468410.
@article{osti_1468410,
title = {X-Ray Properties of SPT Selected Galaxy Clusters at 0.2<z<1.5 Observed with XMM-Newton},
author = {Bulbul, Esra and et al.},
abstractNote = {We present measurements of the X-ray observables of the intra-cluster 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 ($M_{500}\geq 3 \times10^{14}$ $M_\odot$) 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 $\geq 2.5{\sigma}$ significance in the case of $L_X$ and $M_{ICM}$. The redshift trends are consistent with the self-similar expectation in all cases, 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 log-normal intrinsic scatter in the observable at fixed halo mass varies from $\sim$0.10 for $M_{ICM}$ and core-excised $Y_X$ to $\sim$0.27 for core-included bolometric $L_X$. 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 (abridged).},
doi = {},
journal = {Astrophys.J.},
number = ,
volume = ,
place = {United States},
year = {2018},
month = {7}
}