  Knowledge of the structure of galaxy clusters is essential for an
understanding of large scale structure in the universe, and may provide
important clues to the nature of dark matter. Moreover, the shape of the dark
matter distribution in the cluster core may offer insight into the structure
formation process. Unfortunately, cluster cores also tend to be the site of
complicated astrophysics. X-ray imaging spectroscopy of relaxed clusters, a
standard technique for mapping their dark matter distributions, is often
complicated by the presence of cool components in cluster cores, and the dark
matter profile one derives for a cluster is sensitive to assumptions made about
the distribution of this component. In addition, fluctuations in the
temperature measurements resulting from normal statistical variance can produce
results which are unphysical. We present here a procedure for extracting the
dark matter profile of a spherically symmetric, relaxed galaxy cluster which
deals with both of these complications. We apply this technique to a sample of
galaxy clusters observed with the Chandra X-ray Observatory, and comment on the
resulting mass profiles. For some of the clusters we compare their masses with
those derived from weak and strong gravitational measurements.
