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Title: Testing for X-Ray–SZ Differences and Redshift Evolution in the X-Ray Morphology of Galaxy Clusters

Abstract

Here, we present a quantitative study of the X-ray morphology of galaxy clusters, as a function of their detection method and redshift. We analyze two separate samples of galaxy clusters: a sample of 36 clusters at 0.35 < z < 0.9 selected in the X-ray with the ROSAT PSPC 400 deg2 survey, and a sample of 90 clusters at 0.25 < z < 1.2 selected via the Sunyaev-Zel’dovich (SZ) effect with the South Pole Telescope. Clusters from both samples have similar-quality Chandra observations, which allow us to quantify their X-ray morphologies via two distinct methods: centroid shifts (w) and photon asymmetry (Aphot). The latter technique provides nearly unbiased morphology estimates for clusters spanning a broad range of redshift and data quality. We further compare the X-ray morphologies of Xray- and SZ-selected clusters with those of simulated clusters. We do not find a statistically significant difference in the measured X-ray morphology of X-ray and SZ-selected clusters over the redshift range probed by these samples, suggesting that the two are probing similar populations of clusters. We find that the X-ray morphologies of simulated clusters are statistically indistinguishable from those of X-ray- or SZ-selected clusters, implying that the most important physics for dictatingmore » the large-scale gas morphology (outside of the core) is well-approximated in these simulations. Lastly, we find no statistically significant redshift evolution in the X-ray morphology (both for observed and simulated clusters), over the range z ~ 0.3 to z ~ 1, seemingly in contradiction with the redshift-dependent halo merger rate predicted by simulations.« less

Authors:
 [1]; ORCiD logo [2];  [3];  [4]; ORCiD logo [4]; ORCiD logo [5]; ORCiD logo [6];  [7]; ORCiD logo [8];  [7]; ORCiD logo [9];  [10];  [5]; ORCiD logo [11]; ORCiD logo [5]
  1. Harvard Univ., Cambridge, MA (United States)
  2. Massachusetts Inst. of Technology (MIT), Cambridge, MA (United States)
  3. Fermi National Accelerator Lab. (FNAL), Batavia, IL (United States); Univ. of Chicago, Chicago, IL (United States)
  4. Univ. of Chicago, Chicago, IL (United States); Argonne National Lab. (ANL), Argonne, IL (United States)
  5. Harvard-Smithsonian Center for Astrophysics, Cambridge, MA (United States)
  6. Huntingdon Institute for X-Ray Astronomy, Huntingdon, PA (United States)
  7. Ludwig Maximilian Univ., Munich (Germany); Excellence Cluster Universe, Garching (Germany); Max Planck Institute for Extraterrestrial Physics, Garching (Germany)
  8. Univ. de Montreal, Montreal, QC (Canada)
  9. Yale Univ., New Haven, CT (United States)
  10. Univ. of Colorado, Boulder, CO (United States); NASA Ames Research Center, Moffett Field, CA (United States)
  11. Harvard Univ., Cambridge, MA (United States); Harvard-Smithsonian Center for Astrophysics, Cambridge, MA (United States)
Publication Date:
Research Org.:
Argonne National Lab. (ANL), Argonne, IL (United States); Fermi National Accelerator Lab. (FNAL), Batavia, IL (United States)
Sponsoring Org.:
National Aeronautic and Space Administration (NASA); USDOE Office of Science (SC), Basic Energy Sciences (BES) (SC-22); National Science Foundation (NSF); Gordon and Betty Moore Foundation; USDOE Office of Science (SC), High Energy Physics (HEP) (SC-25)
OSTI Identifier:
1373892
Alternate Identifier(s):
OSTI ID: 1373304
Report Number(s):
FERMILAB-PUB-16-701-AE; arXiv:1609.00375
Journal ID: ISSN 1538-4357; 133047
Grant/Contract Number:  
AC02-06CH11357; AC02-07CH11359
Resource Type:
Accepted Manuscript
Journal Name:
The Astrophysical Journal (Online)
Additional Journal Information:
Journal Name: The Astrophysical Journal (Online); Journal Volume: 841; Journal Issue: 1; Journal ID: ISSN 1538-4357
Publisher:
Institute of Physics (IOP)
Country of Publication:
United States
Language:
English
Subject:
79 ASTRONOMY AND ASTROPHYSICS; galaxies: clusters: general; galaxies: clusters: intracluster medium; X-rays: galaxies: clusters

Citation Formats

Nurgaliev, D., McDonald, M., Benson, B. A., Bleem, L., Bocquet, S., Forman, W. R., Garmire, G. P., Gupta, N., Hlavacek-Larrondo, J., Mohr, J. J., Nagai, D., Rapetti, D., Stark, A. A., Stubbs, C. W., and Vikhlinin, A. Testing for X-Ray–SZ Differences and Redshift Evolution in the X-Ray Morphology of Galaxy Clusters. United States: N. p., 2017. Web. doi:10.3847/1538-4357/aa6db4.
Nurgaliev, D., McDonald, M., Benson, B. A., Bleem, L., Bocquet, S., Forman, W. R., Garmire, G. P., Gupta, N., Hlavacek-Larrondo, J., Mohr, J. J., Nagai, D., Rapetti, D., Stark, A. A., Stubbs, C. W., & Vikhlinin, A. Testing for X-Ray–SZ Differences and Redshift Evolution in the X-Ray Morphology of Galaxy Clusters. United States. doi:10.3847/1538-4357/aa6db4.
Nurgaliev, D., McDonald, M., Benson, B. A., Bleem, L., Bocquet, S., Forman, W. R., Garmire, G. P., Gupta, N., Hlavacek-Larrondo, J., Mohr, J. J., Nagai, D., Rapetti, D., Stark, A. A., Stubbs, C. W., and Vikhlinin, A. Tue . "Testing for X-Ray–SZ Differences and Redshift Evolution in the X-Ray Morphology of Galaxy Clusters". United States. doi:10.3847/1538-4357/aa6db4. https://www.osti.gov/servlets/purl/1373892.
@article{osti_1373892,
title = {Testing for X-Ray–SZ Differences and Redshift Evolution in the X-Ray Morphology of Galaxy Clusters},
author = {Nurgaliev, D. and McDonald, M. and Benson, B. A. and Bleem, L. and Bocquet, S. and Forman, W. R. and Garmire, G. P. and Gupta, N. and Hlavacek-Larrondo, J. and Mohr, J. J. and Nagai, D. and Rapetti, D. and Stark, A. A. and Stubbs, C. W. and Vikhlinin, A.},
abstractNote = {Here, we present a quantitative study of the X-ray morphology of galaxy clusters, as a function of their detection method and redshift. We analyze two separate samples of galaxy clusters: a sample of 36 clusters at 0.35 < z < 0.9 selected in the X-ray with the ROSAT PSPC 400 deg2 survey, and a sample of 90 clusters at 0.25 < z < 1.2 selected via the Sunyaev-Zel’dovich (SZ) effect with the South Pole Telescope. Clusters from both samples have similar-quality Chandra observations, which allow us to quantify their X-ray morphologies via two distinct methods: centroid shifts (w) and photon asymmetry (Aphot). The latter technique provides nearly unbiased morphology estimates for clusters spanning a broad range of redshift and data quality. We further compare the X-ray morphologies of Xray- and SZ-selected clusters with those of simulated clusters. We do not find a statistically significant difference in the measured X-ray morphology of X-ray and SZ-selected clusters over the redshift range probed by these samples, suggesting that the two are probing similar populations of clusters. We find that the X-ray morphologies of simulated clusters are statistically indistinguishable from those of X-ray- or SZ-selected clusters, implying that the most important physics for dictating the large-scale gas morphology (outside of the core) is well-approximated in these simulations. Lastly, we find no statistically significant redshift evolution in the X-ray morphology (both for observed and simulated clusters), over the range z ~ 0.3 to z ~ 1, seemingly in contradiction with the redshift-dependent halo merger rate predicted by simulations.},
doi = {10.3847/1538-4357/aa6db4},
journal = {The Astrophysical Journal (Online)},
number = 1,
volume = 841,
place = {United States},
year = {2017},
month = {5}
}

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