Untangling the X-ray emission from the Sa galaxy NGC 1291 with Chandra

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dc.contributor.authorIrwin, JA
dc.contributor.authorSarazin, CL
dc.contributor.authorBregman, JN
dc.contributor.otherUniversity of Michigan System
dc.contributor.otherUniversity of Michigan
dc.contributor.otherUniversity of Virginia
dc.contributor.otherUniversity of Alabama Tuscaloosa
dc.date.accessioned2018-09-14T21:03:47Z
dc.date.available2018-09-14T21:03:47Z
dc.date.issued2002-05-01
dc.description.abstractWe present a Chandra ACIS-S observation of the nearby bulge-dominated Sa galaxy NGC 1291. The X-ray emission from the bulge resembles the X-ray emission from a subclass of elliptical and S0 galaxies with low X-ray-to-optical luminosity ratios. The X-ray emission is composed of a central pointlike nucleus, similar to50 point sources that are most likely low-mass X-ray binaries (LMXBs), and diffuse gas detectable out to a radius of 120" (5.2 kpc). The diffuse gas has a global temperature of 0.32(-0.03)(+0.04) and metallicity of 0.06+/-0.02 solar, and both quantities marginally decrease with increasing radius. The hot gas fills the hole in the H I distribution, and the softening of the spectrum of the X-ray gas with radius might indicate a thermal coupling of the hot and cold phases of the interstellar medium as previously suggested. The integrated X-ray luminosity of the LMXBs, once normalized by the optical luminosity, is a factor of 1.4 less than in the elliptical galaxy NGC 4697 or S0 galaxy NGC 1553. The difference in L-X,L-stellar/L-B between the galaxies appears to be because of a lack of very bright sources in NGC 1291. No sources above 3x10(38) ergs s(-1) were found in NGC 1291 when similar to7 were expected from scaling from NGC 4697 and NGC 1553. The cumulative L-X,L-stellar/L-B value including only sources below 1.0x10(38) ergs s(-1) is remarkably similar between NGC 1291 and NGC 4697, if a recent surface brightness fluctuation-determined distance is assumed for NGC 4697. If this is a common feature of the LMXB population in early-type systems, it might be used as a distance indicator. Finally, a bright, variable [(1.6=3.1) x 10(39) ergs s(-1)] source was detected at the optical center of the galaxy. Its spectrum shows excess soft emission superposed on a highly absorbed power-law component, similar to what has been found in several other low-luminosity active galactic nuclei. However, the soft component does not vary in intensity like the hard component, indicating that the soft component is not reprocessed hard component emission.en_US
dc.format.mimetypeapplication/pdf
dc.identifier.citationIrwin, J., Sarazin, C., Bregman, J. (2002): An Ultraluminous X-Ray Object with a 2 Hour Period in M51. The Astrophysical Journal, 570(1). DOI: 10.1086/339734
dc.identifier.doi10.1086/339734
dc.identifier.orcidhttps://orcid.org/0000-0001-6276-9526
dc.identifier.urihttp://ir.ua.edu/handle/123456789/3867
dc.languageEnglish
dc.language.isoen_US
dc.publisherIOP Publishing
dc.subjectbinaries : close
dc.subjectgalaxies : ISM
dc.subjectX-rays : galaxies
dc.subjectX-rays : ISM
dc.subjectX-rays : stars
dc.subjectCOLD GAS
dc.subjectELLIPTICAL GALAXIES
dc.subjectLENTICULAR GALAXIES
dc.subjectSPECTRAL PROPERTIES
dc.subjectGLOBULAR-CLUSTERS
dc.subjectATOMIC-HYDROGEN
dc.subjectROSAT
dc.subjectHOT
dc.subjectMECHANISMS
dc.subjectSAMPLE
dc.subjectAstronomy & Astrophysics
dc.titleUntangling the X-ray emission from the Sa galaxy NGC 1291 with Chandraen_US
dc.typetext
dc.typeArticle
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