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Please use this identifier to cite or link to this item: http://hdl.handle.net/2289/3629
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dc.contributor.authorNath, Biman B.-
dc.date.accessioned2008-08-04T10:33:15Z-
dc.date.available2008-08-04T10:33:15Z-
dc.date.issued2008-06-
dc.identifier.citationMonthly Notices of the Royal Astronomical Society, 2008, Vol.387, pL50en
dc.identifier.issnE-ISSN: 1365-2966-
dc.identifier.issnP-ISSN: 0035-8711-
dc.identifier.urihttp://hdl.handle.net/2289/3629-
dc.descriptionRestricted Access. An open-access version is available at arXiv.org (one of the alternative locations)en
dc.description.abstractThe distribution of luminous radio galaxies in galaxy clusters has been observed to be concentrated in the inner region. We consider the role of dynamical friction of massive galaxies (M ~ 1012.5Msolar), assuming them to be hosts of luminous radio galaxies, and show that beginning with a Navarro-Frenk-White density profile of a cluster of mass Mcl ~ 1015Msolar of concentration c ~ 5 and collapsing at z ~ 1, the density profile of radio galaxies evolves to a profile of concentration c ~ 25, as observed, in a time-scale of t ~ 3-5 Gyr.en
dc.format.extent490992 bytes-
dc.format.mimetypeapplication/pdf-
dc.language.isoenen
dc.publisherBlackwell Publishing for the RASen
dc.relation.urihttp://adsabs.harvard.edu/abs/2008MNRAS.387L..50Nen
dc.relation.urihttp://arxiv.org/abs/0804.3468en
dc.relation.urihttp://dx.doi.org/10.1111/j.1745-3933.2008.00483.xen
dc.rights2008 The Royal Astronomical Societyen
dc.subjectgalaxies: activeen
dc.subjectgalaxies: clustersen
dc.subjectradio continuum: galaxiesen
dc.titleDynamical friction of radio galaxies in galaxy clustersen
dc.typeArticleen
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