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E. D. Miller, J. N. Bregman (U. Michigan), P. M. Knezek (JHU)
Three important phenomena can produce cool absorbing gas in rich clusters of galaxies: stripping of galactic gas by the hot ambient medium; infall of cool gas into the cluster; and the radiative cooling of the hot gas in the cluster core (cooling flows). Fortunately, each mechanism has a distinctive signature through its spatial distribution and metallicity. We present HST/FOS spectra of five QSOs projected behind both cooling flow and non-cooling flow clusters, with lines of sight ranging from the inner to outer parts of the cluster (0.2 \leq r\rm proj/R\rm cluster \leq 0.7). From non-detections of resonance absorption lines in the 2222--3277 Å\ range, we find 1-\sigma upper limits on the column density of N \leq 1012--1013\ cm-2\ for \ion{Fe}{2}, \ion{Mg}{2}, and \ion{Mn}{2} in each cluster. We discuss the implications of these constraints on the various gas production scenarios.
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