OVI in elliptical galaxies: Indicators of cooling flows

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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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