Heating versus Cooling Galaxies and Clusters of Galaxies: Proceedings the MPA/ESO/MPE/USM Joint Astronomy Conference held Garching, Germany, 6-11 August 2006
Heating versus Cooling Galaxies and Clusters of Galaxies: Proceedings the MPA/ESO/MPE/USM Joint Astronomy Conference held Garching, Germany, 6-11 August 2006 in Chattanooga, TN
Heating versus Cooling Galaxies and Clusters of Galaxies: Proceedings the MPA/ESO/MPE/USM Joint Astronomy Conference held Garching, Germany, 6-11 August 2006 in Chattanooga, TN
The Universe would be a dull and dark place if the gaseous baryons did not cool, collapse, and form stars and galaxies. However, if this gas is allowed to cool unimpeded at the rate predicted from known atomic physics, in the context of a well-established cosmological model, the gaseous matter would form stars and galaxies with a high efficiency, so that far more than the observed fraction of about 10–15% of the baryonic matter would be found in luminous stellar systems. Therefore,cooling must be damped or regulatedby heating processes, and observations show that this ‘feedback’ is a widespread astrophysical phenomenon. The place where this cooling and feedback manifests itself most dram- ically is in the inner regions of the most massive Dark Matter halos found in our Universe, in the cores of galaxy clusters. The effect of cosmic co- ing in these objects was recognized in the mid-1970s, and the term ‘cooling flow’ was introduced by Andy Fabian and colleagues at Cambridge as a p- sible explanation of the physical processes obtained in the central regions of clusters. The name refers to the fact that gas cooling in the inner regions is associated with a loss of central pressure, causing an in?ow of hot gas from larger radii.
The Universe would be a dull and dark place if the gaseous baryons did not cool, collapse, and form stars and galaxies. However, if this gas is allowed to cool unimpeded at the rate predicted from known atomic physics, in the context of a well-established cosmological model, the gaseous matter would form stars and galaxies with a high efficiency, so that far more than the observed fraction of about 10–15% of the baryonic matter would be found in luminous stellar systems. Therefore,cooling must be damped or regulatedby heating processes, and observations show that this ‘feedback’ is a widespread astrophysical phenomenon. The place where this cooling and feedback manifests itself most dram- ically is in the inner regions of the most massive Dark Matter halos found in our Universe, in the cores of galaxy clusters. The effect of cosmic co- ing in these objects was recognized in the mid-1970s, and the term ‘cooling flow’ was introduced by Andy Fabian and colleagues at Cambridge as a p- sible explanation of the physical processes obtained in the central regions of clusters. The name refers to the fact that gas cooling in the inner regions is associated with a loss of central pressure, causing an in?ow of hot gas from larger radii.
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