Abstract
HEAO 1-A2 spectra of clusters of galaxies are used to determine the temperature profile which characterizes the X-ray emitting gas. Strong evidence of non-isothermality is found for the Coma, A85, and A1795 clusters. Properties of the cluster potential which binds the gas are calculated for a range of model parameters. The typical binding mass, if the gas is adiabatic, is 2–4E14 solar masses and is quite centrally concentrated. In addition, the Fe abundance in Coma is .26 ±.06 solar, less than the typical value (.5) found for rich clusters. Our results for the gas in Coma may imply a physical description of the cluster which is quite different from what was previously believed.
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