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We explore the utility of narrow band X-ray surface photometry as a tool formaking fully Bayesian, hydrostatic mass measurements of clusters of galaxies,groups and early-type galaxies. We demonstrate that it is sufficient to measurethe surface photometry with the Chandra X-ray observatory in only three (restframe) bands (0.5--0.9 keV, 0.9--2.0 keV and 2.0--7.0 keV) in order toconstrain the temperature, density and abundance of the hot interstellar medium(ISM). Adopting parametrized models for the mass distribution and radialentropy profile and assuming spherical symmetry, we show that the constraintson the mass and thermodynamic properties of the ISM that are obtained byfitting data from all three bands simultaneously are comparable to thoseobtained by fitting similar models to the temperature and density profilesderived from spatially resolved spectroscopy, as is typically done. Wedemonstrate that the constraints can be significantly tightened when exploitinga recently derived, empirical relationship between the gas fraction and theentropy profile at large scales, eliminating arbitrary extrapolations at largeradii. This "Scaled Adiabatic Model" (ScAM) is well suited to modestsignal-to-noise data, and we show that accurate, precise measurements of theglobal system properties are inferred when employing it to fit data from evenvery shallow, snapshot X-ray observations. The well-defined asymptoticbehaviour of the model also makes it ideally suited for use inSunyaev-Zeldovich studies of galaxy clusters.

Narrow Band X-ray Photometry as a Tool for Studying Galaxy and Cluster Mass Distributions