Models of the ICM with Heating and Cooling: Explaining the Global and Structural X-ray Properties of Clusters

Details Models of the ICM with Heating and Cooling: Explaining the Global and Structural X-ray Properties of Clusters Models of the ICM with Heating and Cooling: Explaining the Global and Structural X-ray Properties of Clusters

2004-06-14

arxiv.org/abs/astro-ph/0406329v1

Astrophys.J. 613 (2004) 811-830

Astronomy and Astrophysics

Astrophysics

20 pages, 15 figures, accepted for publication in the Astrophysical Journal

Scientific paper

10.1086/423267

(Abridged) Theoretical models that include only gravitationally-driven processes fail to match the observed mean X-ray properties of clusters. As a result, there has recently been increased interest in models in which either radiative cooling or entropy injection play a central role in mediating the properties of the intracluster medium. Both sets of models give reasonable fits to the mean properties of clusters, but cooling only models result in fractions of cold baryons in excess of observationally established limits and the simplest entropy injection models do not treat the "cooling core" structure present in many clusters and cannot account for entropy profiles revealed by recent X-ray observations. We consider models that marry radiative cooling with entropy injection, and confront model predictions for the global and structural properties of massive clusters with the latest X-ray data. The models successfully and simultaneously reproduce the observed L-T and L-M relations, yield detailed entropy, surface brightness, and temperature profiles in excellent agreement with observations, and predict a cooled gas fraction that is consistent with observational constraints. The model also provides a possible explanation for the significant intrinsic scatter present in the L-T and L-M relations and provides a natural way of distinguishing between clusters classically identified as "cooling flow" clusters and dynamically relaxed "non-cooling flow" clusters. The former correspond to systems that had only mild levels (< 300 keV cm^2) of entropy injection, while the latter are identified as systems that had much higher entropy injection. This is borne out by the entropy profiles derived from Chandra and XMM-Newton.

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