Testing for X-Ray–SZ Differences and Redshift Evolution in the X-Ray Morphology of Galaxy Clusters
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- Harvard Univ., Cambridge, MA (United States)
- Massachusetts Inst. of Technology (MIT), Cambridge, MA (United States)
- Fermi National Accelerator Lab. (FNAL), Batavia, IL (United States); Univ. of Chicago, Chicago, IL (United States)
- Univ. of Chicago, Chicago, IL (United States); Argonne National Lab. (ANL), Argonne, IL (United States)
- Harvard-Smithsonian Center for Astrophysics, Cambridge, MA (United States)
- Huntingdon Institute for X-Ray Astronomy, Huntingdon, PA (United States)
- Ludwig Maximilian Univ., Munich (Germany); Excellence Cluster Universe, Garching (Germany); Max Planck Institute for Extraterrestrial Physics, Garching (Germany)
- Univ. de Montreal, Montreal, QC (Canada)
- Yale Univ., New Haven, CT (United States)
- Univ. of Colorado, Boulder, CO (United States); NASA Ames Research Center, Moffett Field, CA (United States)
- Harvard Univ., Cambridge, MA (United States); Harvard-Smithsonian Center for Astrophysics, Cambridge, MA (United States)
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 $$0.35\lt z\lt 0.9$$ selected in the X-ray with the ROSAT PSPC 400 deg(2) survey, and a sample of 90 clusters at $$0.25\lt z\lt 1.2$$ 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 ($${A}_{\mathrm{phot}}$$). 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 X-ray- 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. Finally, we find no statistically significant redshift evolution in the X-ray morphology (both for observed and simulated clusters), over the range of $$z\sim 0.3$$ to $$z\sim 1$$, seemingly in contradiction with the redshift-dependent halo merger rate predicted by simulations.
- Research Organization:
- Argonne National Lab. (ANL), Argonne, IL (United States); Fermi National Accelerator Lab. (FNAL), Batavia, IL (United States)
- Sponsoring Organization:
- National Aeronautics and Space Administration (NASA); USDOE Office of Science (SC), Basic Energy Sciences (BES); National Science Foundation (NSF); Gordon and Betty Moore Foundation; USDOE Office of Science (SC), High Energy Physics (HEP)
- Grant/Contract Number:
- AC02-06CH11357; AC02-07CH11359
- OSTI ID:
- 1373892
- Alternate ID(s):
- OSTI ID: 1373304
- Report Number(s):
- FERMILAB-PUB-16-701-AE; arXiv:1609.00375; 133047
- Journal Information:
- The Astrophysical Journal (Online), Vol. 841, Issue 1; ISSN 1538-4357
- Publisher:
- Institute of Physics (IOP)Copyright Statement
- Country of Publication:
- United States
- Language:
- English
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