An X-ray size-temperature relation for galaxy clusters: Observation and simulation
dc.contributor.author | Mohr, J. J. | en_US |
dc.contributor.author | Evrard, August E. | en_US |
dc.date.accessioned | 2008-08-14T19:11:14Z | |
dc.date.available | 2008-08-14T19:11:14Z | |
dc.date.issued | 1997-12-10 | en_US |
dc.identifier.citation | Mohr, JJ; Evrard, AE. (1997). Astrophysical Journal, 491:(1, Part1) 38-44. <http://hdl.handle.net/2027.42/60594> | en_US |
dc.identifier.issn | 0004-637X | en_US |
dc.identifier.uri | http://arxiv.org/abs/astro-ph/9707184 | en_US |
dc.identifier.uri | https://hdl.handle.net/2027.42/60594 | |
dc.description.abstract | We show that galaxy clusters conform to a tight relation between X-ray isophotal size R-I and emission-weighted intracluster medium (ICM) temperature [T-X]. The best-fit relation for 41 members of an X-ray flux-limited cluster sample is log R-I = (0.93 +/- 0.11) log ([T-X]/6 keV)-(0.08 +/- 0.01); intrinsic scatter in size about the relation is 15%, and for 30 clusters with [T-X] > 4 keV, the scatter is reduced to 10%. The existence of the size-temperature (ST) relation indicates that the ICM structure is a well-behaved function of [T-X]. We use an ensemble of gasdynamic simulations to demonstrate that a cluster population experiencing present-epoch growth nevertheless conforms to an ST relation with scatter similar to that observed; the simulations also exhibit a tight relation between M-vir and [T-X], providing the suggestion that a similar relation holds for observed clusters. We use the scatter in R, to estimate limits on the rms variation in ICM mass fraction delta f(ICM) at constant [T-X]: delta f/f(ICM) less than or equal to 22% (less than or equal to 14% for clusters with [T-X] > 4 keV). It appears that a mechanism like feedback from galactic winds, which introduces systematic structural changes in the ICM, is required to reproduce the observed slope of the ST relation. | en_US |
dc.format.extent | 228539 bytes | |
dc.format.extent | 18 bytes | |
dc.format.mimetype | application/pdf | |
dc.format.mimetype | text/plain | |
dc.publisher | Univ Chicago Press | en_US |
dc.subject | Galaxies : Clusters : General | en_US |
dc.subject | Intergalactic Medium | en_US |
dc.subject | X-rays : Galaxies | en_US |
dc.title | An X-ray size-temperature relation for galaxy clusters: Observation and simulation | en_US |
dc.type | Article | en_US |
dc.subject.hlbsecondlevel | Physics | en_US |
dc.subject.hlbtoplevel | Science | en_US |
dc.description.peerreviewed | Peer Reviewed | en_US |
dc.contributor.affiliationother | UNIV MICHIGAN,DEPT ASTRON,ANN ARBOR,MI 48109 | en_US |
dc.contributor.affiliationother | INST ASTROPHYS,F-75014 PARIS,FRANCE | en_US |
dc.contributor.affiliationumcampus | Ann Arbor | en_US |
dc.description.bitstreamurl | http://deepblue.lib.umich.edu/bitstream/2027.42/60594/1/MohrEvrard1997X-ray.pdf | |
dc.identifier.doi | http://dx.doi.org/10.1086/304957 | en_US |
dc.owningcollname | Astrophysics (Physics, Department of) |
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