Tracing the Gas to the Virial Radius (R_{100}) in a Galaxy Group

Details Tracing the Gas to the Virial Radius (R_{100}) in a Galaxy Group Tracing the Gas to the Virial Radius (R_{100}) in a Galaxy Group

Aug 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011scgg.conf...24h&link_type=abstract

"Structure in Clusters and Groups of Galaxies in the Chandra Era, 2011 Chandra Science Workshop held July 12-14, 2011. Edited by

Mathematics

Logic

Scientific paper

We present a Chandra and Suzaku study of the fossil group/ poor cluster RXJ1159+5531. The Chandra data reveals a round, relaxed morphology, while the combination of flat surface brightness profile, high luminosity and optimal distance allow the ICM to be detected to the virial radius (R_{100}=1.1Mpc) in a single Suzaku field. We measure the gas over ˜3 orders of magnitude in radius. With 4 data-bins beyond 0.5R_{200} and good azimuthal coverage (>30%), we find no evidence that the entropy profile flattens at large scales (>R_{500}). The baryon fraction within R_{100} is consistent with the Cosmological value (0.15±0.02). This contrasts sharply with recent results for Virgo and Perseus, indicating that substantial gas clumping cannot be ubiquitous, at least in highly evolved clusters.

Affiliated with

Also associated with

No associations

Rating

Tracing the Gas to the Virial Radius (R_{100}) in a Galaxy Group does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.

If you have personal experience with Tracing the Gas to the Virial Radius (R_{100}) in a Galaxy Group, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Tracing the Gas to the Virial Radius (R_{100}) in a Galaxy Group will most certainly appreciate the feedback.

Rate now

Comments { 0 }

Profile ID: LFWR-SCP-O-1667430