[Previous] | [Session 51] | [Next]
M. W. Wise, J. C. Houck (MIT)
The lack of strong emission lines from gas at temperatures below 3 keV in XMM RGS and Chandra HETG spectra has become a key argument for cooling flow models which include such additional physics as AGN heating, thermal conduction, star formation, and internal absorption. Due to observational limitations, RGS and HETG spectroscopy is however typically limited to studying the cooling flow spectrum from the cluster as a whole. Alternatively, Chandra ACIS imaging of clusters can sample the cluster temperature structure in the core directly albeit at reduced spectral resolution. We present the results from a spatially resolved, spectral analysis of the Perseus cooling flow cluster. Using a simple, parameterized differential emission measure model, we have determined the departures from the canonical, isobaric cooling flow model for each cluster, both globally and as a function of position in the cluster. We present maps of the heating in the Perseus cluster and discuss their implications for modified cooling flow models which include heating and absorption.
[Previous] | [Session 51] | [Next]
Bulletin of the American Astronomical Society, 35#5
© 2003. The American Astronomical Soceity.