What is a Cool-Core Cluster? A Detailed Analysis of the Cores of the X-ray Flux-Limited HIFLUGCS Cluster Sample Export

@article{citeulike:6066208, abstract = {We use the largest complete sample of 64 galaxy clusters (HIghest X-ray FLUx Galaxy Cluster Sample) with available high-quality X-ray data from Chandra, and apply 16 cool-core diagnostics to them, some of them new. We also correlate optical properties of brightest cluster galaxies (BCGs) with X-ray properties. To segregate cool core and non-cool-core clusters, we find that central cooling time, t\_cool, is the best parameter for low redshift clusters with high quality data, and that cuspiness is the best parameter for high redshift clusters. 72\% of clusters in our sample have a cool core (t\_cool \< 7.7 h\_{71}^{-1/2} Gyr) and 44\% have strong cool cores (t\_cool \<1.0 h\_{71}^{-1/2} Gyr). For the first time we show quantitatively that the discrepancy in classical and spectroscopic mass deposition rates can not be explained with a recent formation of the cool cores, demonstrating the need for a heating mechanism to explain the cooling flow problem. [Abridged]}, archivePrefix = {arXiv}, author = {Hudson, Daniel S. and Mittal, Rupal and Reiprich, Thomas H. and Nulsen, Paul E. J. and Andernach, Heinz and Sarazin, Craig L.}, citeulike-article-id = {6066208}, citeulike-linkout-0 = {http://arxiv.org/abs/0911.0409}, citeulike-linkout-1 = {http://arxiv.org/pdf/0911.0409}, day = {2}, eprint = {0911.0409}, keywords = {clusters, cool-core, observations, x-ray}, month = {Nov}, posted-at = {2009-11-04 03:13:38}, priority = {2}, title = {What is a Cool-Core Cluster? A Detailed Analysis of the Cores of the X-ray Flux-Limited HIFLUGCS Cluster Sample}, url = {http://arxiv.org/abs/0911.0409}, year = {2009} }

TY - JOUR ID - citeulike:6066208 L3 - citeulike-article-id:6066208 N2 - We use the largest complete sample of 64 galaxy clusters (HIghest X-ray FLUx Galaxy Cluster Sample) with available high-quality X-ray data from Chandra, and apply 16 cool-core diagnostics to them, some of them new. We also correlate optical properties of brightest cluster galaxies (BCGs) with X-ray properties. To segregate cool core and non-cool-core clusters, we find that central cooling time, t_cool, is the best parameter for low redshift clusters with high quality data, and that cuspiness is the best parameter for high redshift clusters. 72% of clusters in our sample have a cool core (t_cool < 7.7 h_{71}^{-1/2} Gyr) and 44% have strong cool cores (t_cool <1.0 h_{71}^{-1/2} Gyr). For the first time we show quantitatively that the discrepancy in classical and spectroscopic mass deposition rates can not be explained with a recent formation of the cool cores, demonstrating the need for a heating mechanism to explain the cooling flow problem. [Abridged] TI - What is a Cool-Core Cluster? A Detailed Analysis of the Cores of the X-ray Flux-Limited HIFLUGCS Cluster Sample KW - clusters KW - cool-core KW - observations KW - x-ray AU - Hudson, Daniel AU - Mittal, Rupal AU - Reiprich, Thomas AU - Nulsen, Paul AU - Andernach, Heinz AU - Sarazin, Craig PY - 2009/Nov/02/ UR - http://arxiv.org/abs/0911.0409 ER -