OVI in elliptical galaxies: Indicators of cooling flows

dc.contributor.authorBregman, JN
dc.contributor.authorMiller, ED
dc.contributor.authorAthey, AE
dc.contributor.authorIrwin, JA
dc.contributor.otherUniversity of Michigan System
dc.contributor.otherUniversity of Michigan
dc.contributor.otherMassachusetts Institute of Technology (MIT)
dc.contributor.otherCarnegie Institution for Science
dc.contributor.otherUniversity of Alabama Tuscaloosa
dc.date.accessioned2018-09-14T13:22:50Z
dc.date.available2018-09-14T13:22:50Z
dc.date.issued2005-12-20
dc.description.abstractEarly-type galaxies often contain a hot X-ray-emitting interstellar medium [(3-8) x 10(6) K] with an apparent radiative cooling time much less than a Hubble time. If unopposed by a heating mechanism, the gas will radiatively cool to temperatures less than or similar to 10(4) K at a rate proportional to L-X/T-X, typically 0.03-1 M-circle dot yr(-1). We can test whether gas is cooling through the 3 x 10(5) K range by observing the O VI doublet, whose luminosity is proportional to the cooling rate. Here we report on a study of an unbiased sample of 24 galaxies, obtaining Far Ultraviolet Spectroscopic Explorer spectra to complement the X-ray data of ROSAT and Chandra. The O VI line emission was detected in about 40% of the galaxies and at a luminosity level similar to the prediction from the cooling flow model. There is a correlation between. M-O (VI) and M-X, although there is significant dispersion about the relationship, where the O VI is brighter or dimmer than expected by a factor of 3 or more. If the cooling flow picture is to be retained, then this dispersion requires that cooling flows be time-dependent, as might occur by the activity of an AGN. However, of detected objects, those with the highest or lowest values of. M-O (VI)/M-X are not systematically hot or cool, as one might predict from AGN heating.en_US
dc.format.mimetypeapplication/pdf
dc.identifier.citationBregman, J., Miller, E., Athey, A., Irwin, J. (2005): O VI In Elliptical Galaxies: Indicators of Cooling Flows The Astrophysical Journal, 635(2). DOI: 10.1086/497421
dc.identifier.doi10.1086/497421
dc.identifier.urihttp://ir.ua.edu/handle/123456789/3856
dc.languageEnglish
dc.language.isoen_US
dc.publisherIOP Publishing
dc.subjectcooling flows
dc.subjectgalaxies : ISM
dc.subjectultraviolet : galaxies
dc.subjectX-rays : galaxies
dc.subjectX-RAY-EMISSION
dc.subjectINTERSTELLAR MATTER
dc.subjectINFRARED-EMISSION
dc.subjectSUPERNOVA RATES
dc.subjectXMM-NEWTON
dc.subjectMASS-LOSS
dc.subjectHOT GAS
dc.subjectCATALOG
dc.subjectMODELS
dc.subjectAstronomy & Astrophysics
dc.titleOVI in elliptical galaxies: Indicators of cooling flowsen_US
dc.typetext
dc.typeArticle
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