Constraints on Cool Gas in Rich Clusters of Galaxies | Zendy

Eric D. Miller | Zendy; Joel N. Bregman | Zendy; P. M. Knezek | Zendy

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Constraints on Cool Gas in Rich Clusters of Galaxies

Author(s) -

Eric D. Miller,

Joel N. Bregman,

P. M. Knezek

Publication year - 2002

Publication title -

the astrophysical journal

Language(s) - English

Resource type - Journals

SCImago Journal Rank - 2.376

H-Index - 489

eISSN - 1538-4357

pISSN - 0004-637X

DOI - 10.1086/339235

Subject(s) - physics , astrophysics , intracluster medium , quasar , cooling flow , galaxy cluster , galaxy , redshift , cluster (spacecraft) , active galactic nucleus , line of sight , astronomy , ionization , stripping (fiber) , absorption (acoustics) , ion , optics , computer science , electrical engineering , programming language , engineering , quantum mechanics

Cool gas should be present in galaxy clusters due to stripping of galacticgas, infall onto the cluster, and from cooling flows. We searched for this gasthrough resonance absorption line observations from low-ionization metal linegas toward six background quasars. Both cooling flow and non-cooling flowclusters were observed, with lines of sight from the inner to outer parts ofthe cluster (0.2 <= r_proj/R_cluster <= 0.7). The HST/FOS spectra failed todetect Fe II or Mg II absorption at the cluster redshift, with 1-sigma upperlimits on the ion column densities of N <= 10^12 - 10^13 cm^-2. The failure todetect absorption lines implies that the cool cluster gas either is more highlyionized or it has a low covering factor.

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