Constraints on Cool Gas in Rich Clusters of Galaxies

Details Constraints on Cool Gas in Rich Clusters of Galaxies Constraints on Cool Gas in Rich Clusters of Galaxies

Apr 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002apj...569..134m&link_type=abstract

The Astrophysical Journal, Volume 569, Issue 1, pp. 134-143.

Astronomy and Astrophysics

Astronomy

5

Galaxies: Clusters: General, Galaxies: Quasars: Absorption Lines

Scientific paper

Cool gas should be present in galaxy clusters due to stripping of galactic gas, in-fall onto the cluster, and from cooling flows. We have searched for this gas through metal resonance absorption lines from low-ionization gas toward six background quasars. Both cooling-flow and non-cooling-flow clusters were observed, with lines of sight ranging from the inner to outer parts of the cluster (0.32Mpc<=rproj<=1.40Mpc). The HST Faint Object Spectrograph observations failed to detect Fe II or Mg II absorption at the cluster redshift, with 1 σ upper limits on the ion column densities of N<=1012-1013 cm-2. From existing X-ray data, we estimate that ram-pressure stripping of galactic gas by the intracluster medium should produce cool gas along these sight lines. The failure to detect absorption lines implies that any gas stripped in such a way has a low covering fraction, possibly due to a short lifetime in this low-ionization state.

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