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Correlated multiwavelength emission from the X-ray-bright Seyfert galaxy III Zw 2
dc.contributor.authorSalvi, N. J.en_US
dc.contributor.authorPage, M. J.en_US
dc.contributor.authorStevens, J. A.en_US
dc.contributor.authorWu, K.en_US
dc.contributor.authorMason, K. O.en_US
dc.contributor.authorAller, Margo F.en_US
dc.contributor.authorAller, Hugh D.en_US
dc.contributor.authorTeräsranta, H.en_US
dc.contributor.authorRomero-Colmenero, E.en_US
dc.contributor.authorCordova, F. A.en_US
dc.contributor.authorPriedhorsky, William C.en_US
dc.date.accessioned2010-06-01T20:38:03Z
dc.date.available2010-06-01T20:38:03Z
dc.date.issued2002-09en_US
dc.identifier.citationSalvi, N. J.; Page, M. J.; Stevens, J. A.; Wu, K.; Mason, K. O.; Aller, M. F.; Aller, H. D.; TerÄsranta, H.; Romero-Colmenero, E.; Cordova, F. A.; Priedhorsky, W. C. (2002). "Correlated multiwavelength emission from the X-ray-bright Seyfert galaxy III Zw 2." Monthly Notices of the Royal Astronomical Society 335(1): 177-188. <http://hdl.handle.net/2027.42/73740>en_US
dc.identifier.issn0035-8711en_US
dc.identifier.issn1365-2966en_US
dc.identifier.urihttps://hdl.handle.net/2027.42/73740
dc.description.abstractThe X-ray-bright Seyfert 1 galaxy III Zw 2 was observed with XMM–Newton in 2000 July. Its X-ray spectrum can be described by a power law of photon index Γ= 1.7 and an extremely broad (FWHM∼ 140 000 km s −1 ) Fe KΑ line at 6.44 keV. The iron line has an equivalent width of ∼800 eV. To study the long-term X-ray behaviour of the source we have analysed 25 yr of data, from 1975 to 2000. There is no evidence of significant intrinsic absorption within the source or of a soft X-ray excess in the XMM or archival data. We do not detect rapid X-ray variability (a few × 10 3 s ) during any of the individual observations; however, on longer time-scales (a few years) the X-ray light curve shows 10-fold flux variations. We infer a black hole mass of ∼10 9 M ⊙ (from HΒ FWHM) for III Zw 2 which is much higher than some previous estimates. A comparison of X-ray variability with light curves at other wavelengths over a 25-yr period reveals correlated flux variations from radio to X-ray wavelengths. We interpret the variable radio to optical emission as synchrotron radiation, self-absorbed in the radio/millimetre region, and the X-rays mainly as a result of Compton up-scattering of low-energy photons by the population of high-energy electrons that give rise to the synchrotron radiation.en_US
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dc.format.extent3109 bytes
dc.format.mimetypeapplication/pdf
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dc.publisherBlackwell Science Ltden_US
dc.rightsRASen_US
dc.subject.otherAccretionen_US
dc.subject.otherAccretion Discsen_US
dc.subject.otherGalaxies: Activeen_US
dc.subject.otherGalaxies: Nucleien_US
dc.subject.otherQuasars: Generalen_US
dc.subject.otherQuasars: Individual: III Zw 2en_US
dc.titleCorrelated multiwavelength emission from the X-ray-bright Seyfert galaxy III Zw 2en_US
dc.typeArticleen_US
dc.subject.hlbsecondlevelAstronomyen_US
dc.subject.hlbtoplevelScienceen_US
dc.description.peerreviewedPeer Revieweden_US
dc.contributor.affiliationumAstronomy Department, University of Michigan, Ann Arbour, MI 48109-1090, USAen_US
dc.contributor.affiliationotherMullard Space Science Laboratory, University College London, Holmbury St Mary, Dorking, Surrey RH5 6NTen_US
dc.contributor.affiliationotherAstronomy Technology Centre, Royal Observatory, Blackford Hill, Edinburgh EH9 3HJen_US
dc.contributor.affiliationotherMetsÄhovi Radio Observatory, MetsÄhovintie, FIN-02540 KylmÄlÄ, Finlanden_US
dc.contributor.affiliationotherSouth African Astronomical Observatory, PO Box 9, Observatory 7935, South Africaen_US
dc.contributor.affiliationotherDepartment of Physics, University of California, Santa Barbara, CA 93106, USAen_US
dc.contributor.affiliationotherNIS Division, Los Alamos National Laboratory, Los Alamos, NM 87545, USAen_US
dc.description.bitstreamurlhttp://deepblue.lib.umich.edu/bitstream/2027.42/73740/1/j.1365-8711.2002.05603.x.pdf
dc.identifier.doi10.1046/j.1365-8711.2002.05603.xen_US
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