期刊
ASTROPHYSICAL JOURNAL
卷 841, 期 1, 页码 -出版社
IOP PUBLISHING LTD
DOI: 10.3847/1538-4357/aa6db4
关键词
galaxies: clusters: general; galaxies: clusters: intracluster medium; X-rays: galaxies: clusters
资金
- NASA [13800883, 16800690, GO213004B]
- National Science Foundation [ANT-0638937, PLR-1248097]
- U.S. Department of Energy [DE-AC02-06CH11357]
- Fermi Research Alliance, LLC [De-AC02-07CH11359]
- NSF Physics Frontier Center [PHY-0114422]
- Kavli Foundation
- Gordon and Betty Moore Foundation
- NSF [AST-1412768]
- NASA at the NASA Ames Research Center
- NASA
- United States Department of Energy
- Direct For Mathematical & Physical Scien
- Division Of Physics [1125897] Funding Source: National Science Foundation
- Directorate For Geosciences
- Office of Polar Programs (OPP) [1248097] Funding Source: National Science Foundation
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 deg(2) 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 (A(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 similar to 0.3 to z similar to 1, seemingly in contradiction with the redshift-dependent halo merger rate predicted by simulations.
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