Journal
ASTROPHYSICAL JOURNAL
Volume 774, Issue 1, Pages -Publisher
IOP PUBLISHING LTD
DOI: 10.1088/0004-637X/774/1/23
Keywords
early universe; galaxies: clusters: general; galaxies: clusters: intracluster medium; X-rays: galaxies: clusters
Categories
Funding
- NASA [HST-HF51308.01-A, 12800071, 12800088, 13800883]
- Space Telescope Science Institute
- Association of Universities for Research in Astronomy, Inc., for NASA [NAS 5-26555]
- National Science Foundation [ANT-0638937]
- NSF Physics Frontier Center [PHY-0114422]
- Kavli Foundation
- Gordon and Betty Moore Foundation
- NSF [AST-1009012, AST-1009649, MRI-0723073]
- U.S. Department of Energy [DE-AC02-06CH11357]
- Direct For Mathematical & Physical Scien [1009649] Funding Source: National Science Foundation
- Directorate For Geosciences [1248097] Funding Source: National Science Foundation
- Division Of Astronomical Sciences [1009012] Funding Source: National Science Foundation
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We present first results on the cooling properties derived from Chandra X-ray observations of 83 high-redshift (0.3 < z < 1.2) massive galaxy clusters selected by their Sunyaev-Zel'dovich signature in the South Pole Telescope data. We measure each cluster's central cooling time, central entropy, and mass deposition rate, and compare these properties to those for local cluster samples. We find no significant evolution from z similar to 0 to z similar to 1 in the distribution of these properties, suggesting that cooling in cluster cores is stable over long periods of time. We also find that the average cool core entropy profile in the inner similar to 100 kpc has not changed dramatically since z similar to 1, implying that feedback must be providing nearly constant energy injection to maintain the observed entropy floor at similar to 10 keV cm(2). While the cooling properties appear roughly constant over long periods of time, we observe strong evolution in the gas density profile, with the normalized central density (rho(g),(0)/rho(crit)) increasing by an order of magnitude from z similar to 1 to z similar to 0. When using metrics defined by the inner surface brightness profile of clusters, we find an apparent lack of classical, cuspy, cool-core clusters at z > 0.75, consistent with earlier reports for clusters at z > 0.5 using similar definitions. Our measurements indicate that cool cores have been steadily growing over the 8 Gyr spanned by our sample, consistent with a constant, similar to 150M(circle dot) yr(-1) cooling flow that is unable to cool below entropies of 10 keV cm(2) and, instead, accumulates in the cluster center. We estimate that cool cores began to
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