A ROSAT PSPC observations of the lensing clutser A1689

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Abstract
Using the surface brightness distribution from the ROSAT PSPC and the Ginga broad‐beam temperature, we derive a range of acceptable potentials for the cluster A1689. The faint optical arcs observed in A1689 lie at radii which are too large to be produced by simple smooth potentials, consistent with the X‐ray data and with plausible elongation along the line‐of‐sight. They thus reflect superposition or substructure. Although the x‐ray observations show no evidence of substructure, the cluster velocity dispersion is too large to be due to a single cluster with the gas temperature and mass measured through the X‐ray observations. The galaxy radial velocity data then suggest the superposition of one or more subclusters directly along the line‐of‐sight to the primary A1689 cluster. The cooling flow region in the cluster core is well resolved by the PSPC. Spectral fitting of the inner 1′ shows emission from gas cooler than the broad‐beam temperature, and consistent with a massive cooling flow of ≊500 M ⊙ yr− 1, in agreement with the mass deposition rate found from a deprojection analysis of the imaging data.

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