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"abstractNote": "Shortly after the first results of Chandra and XMM-Newton appeared, many researchers in the field abandoned the term \"cooling flow clusters\" in favor of the name \"cool core clusters\". This change, I argue, has been causing damage by promoting the view that there is no substantial cooling in these clusters. In this contribution I discuss the following points, with emphasize on the last one that deals with magnetic fields in cooling flow clusters. (1) Both AGN-feedback and hot-gas cooling to form stars occur during galaxy formation as well as in cooling flow clusters. Ignoring cooling of the intra-cluster medium, as implied by the term \"cool core\", does not encourage comparative study of AGN feedback in cooling flow clusters with that of galaxy formation. (2) The line of thought that there is no cooling might lead to wrong questions and research directions. (3) A key question in both cooling flow clusters and during galaxy formation is the mode of accretion by the super massive black hole (SMBH). When cooling is neglected only accretion from the hot phase remains. Accretion from the hot phase, such as the Bondi accretion, suffers from some severe problems. (4) When it is accepted that moderate quantities of gas are cooling, it becomes clear that global heat conduction must be substantially suppressed. This does not favor a globally ordered magnetic field. As well, it makes global heat conduction unattractive.",
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"abstractNote": "Context: A study of the structural and scaling properties of the temperature distribution of the hot, X-ray emitting intra-cluster medium of galaxy clusters, and its dependence on dynamical state, can give insights into the physical processes governing the formation and evolution of structure.\nAims: Accurate temperature measurements are a pre-requisite for a precise knowledge of the thermodynamic properties of the intra-cluster medium.\nMethods: We analyse the X-ray temperature profiles from XMM-Newton observations of 15 nearby (z<0.2) clusters, drawn from a statistically representative sample. The clusters cover a temperature range from 2.5 keV to 8.5 keV, and present a variety of X-ray morphologies. We derive accurate projected temperature profiles to ~ 0.5 R200, and compare structural properties (outer slope, presence of cooling core) with a quantitative measure of the X-ray morphology as expressed by power ratios. We also compare the results to recent cosmological numerical simulations.\nResults: Once the temperature profiles are scaled by an average cluster temperature (excluding the central region) and the estimated virial radius, the profiles generally decline in the region 0.1 R200 ⪉ R ⪉ 0.5 R200. The central regions show the largest scatter, attributable mostly to the presence of cool core clusters. There is good agreement with numerical simulations outside the core regions. We find no obvious correlations between power ratio and outer profile slope. There may however be a weak trend with the existence of a cool core, in the sense that clusters with a central temperature decrement appear to be slightly more regular.\nConclusions: .The present results lend further evidence to indicate that clusters are a regular population, at least outside the core region.",
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