Formation of cold molecular filaments in cooling flow clusters

Details Formation of cold molecular filaments in cooling flow clusters Formation of cold molecular filaments in cooling flow clusters

2006-10-31

arxiv.org/abs/astro-ph/0610950v1

Astronomy and Astrophysics

Astrophysics

3 pages, 4 figures, To appear in the Proceedings of "Heating vs. Cooling in Galaxies and Clusters of Galaxies", August 2006, G

Scientific paper

New CO observations at the center of cooling flow in Perseus cluster \cite{salome06} show a clear correlation of the molecular gas with the previously detected H-$\alpha$ filaments \cite{conselice01}. In this poster, we present high resolution multi-phase simulations of the Perseus Cluster, taking into account the AGN feedback in form of hot buoyant bubbles. These simulations show that significant amount of gas can cool far from the center. The AGN feedback provides some heating, but also trigger the hot gas compression, that favours cooling (positive feedback), even at high radius ($R>30 \rm{kpc}$). The cooled gas flows into the cluster core forming the observed filaments.

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