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E. D. Sidman, J. C. Kempner (Bowdoin College), L. P. David (Harvard-Smithsonian Center for Astrophysics)
The large scatter in the X-ray luminosity-temperature relation among 2--4 keV clusters indicates a significant deviation from self-similar models of cluster formation. This requires a source or sources of non-gravitational heating of the ICM, such as AGN heating, mergers, or supernova ``pre-heating.'' We present high angular resolution temperature and abundance maps of a sample of bright, nearby poor clusters in this energy range. Substructures in the temperature maps are used to distinguish between different forms of energy injection into the ICM with greater precision than purely radial profiles, while the abundance maps are used to probe inhomogeneities in the distribution of metals in the ICM as well as the relative contributions of type I and type II supernovae to the metal content. Support for this work was provided by the National Aeronautics and Space Administration through Chandra Award Number G05-5138A issued by the Chandra X-ray Observatory Center, which is operated by the Smithsonian Astrophysical Observatory for and on behalf of NASA under contract NAS8-39073, and by NASA contract NAG5-12933.
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Bulletin of the American Astronomical Society, 37 #4
© 2005. The American Astronomical Soceity.