Show simple item record

dc.contributorVirginia Techen
dc.contributor.authorDi Gesu, L.en
dc.contributor.authorArav, Nahumen
dc.contributor.authorBorguet, B.en
dc.contributor.authorDetmers, R. G.en
dc.contributor.authorEbrero, J.en
dc.contributor.authorEdmonds, Douglasen
dc.contributor.authorKaastra, J. S.en
dc.contributor.authorPiconcelli, E.en
dc.contributor.authorVerbunt, F.en
dc.contributor.authorConstantini, E.en
dc.date.accessioned2013-12-06T13:58:47Zen
dc.date.available2013-12-06T13:58:47Zen
dc.date.issued2013-08en
dc.identifier.citationDi Gesu, L. ; Costantini, E. ; Arav, N. ; et al., Aug. 2013. “Simultaneous XMM-Newton and HST-COS observation of 1H0419-577 The absorbing and emitting ionized gas,” ASTRONOMY & ASTROPHYSICS 556:A94. DOI: 10.1051/0004-6361/201321416en
dc.identifier.issn0004-6361en
dc.identifier.urihttp://hdl.handle.net/10919/24433en
dc.description.abstractIn this paper we analyze the X-ray, UV, and optical data of the Seyfert 1.5 galaxy 1H0419-577 with the aim of detecting and studying an ionized-gas outflow. The source was observed simultaneously in the X-rays with XMM-Newton and in the UV with HST-COS. Optical data were also acquired with the XMM-Newton Optical Monitor. We detected a thin, lowly ionized warm absorber (log xi approximate to 0.03, log N-H approximate to 19.9 cm(-2)) in the X-ray spectrum, which is consistent to be produced by the same outflow already detected in the UV. Provided the gas density estimated in the UV, the outflow is consistent to be located in the host galaxy at similar to kpc scale. Narrow emission lines were detected in the X-rays, in the UV and also in the optical spectrum. A single photoionized-gas model cannot account for all the narrow lines emission, indicating that the narrow line region is probably a stratified environment, differing in density and ionization. X-ray lines are unambiguously produced in a more highly ionized gas phase than the one emitting the UV lines. The analysis also suggests that the X-ray emitter may just be a deeper portion of the same gas layer producing the UV lines. Optical lines are probably produced in another disconnected gas system. The different ionization condition and the similar to pc scale location, suggested by the line width for the narrow lines emitters, are evidences against a connection between the warm absorber and the narrow line region in this source.en
dc.description.sponsorshipESA Member Statesen
dc.description.sponsorshipUSA (NASA)en
dc.description.sponsorshipNWO, the Netherlands Organization for Scientific Researchen
dc.description.sponsorshipNASA NNX09AT29G, HST-GO-11686en
dc.language.isoen_USen
dc.publisherEDP Sciencesen
dc.rightsIn Copyrighten
dc.rights.urihttp://rightsstatements.org/vocab/InC/1.0/en
dc.subjectgalaxies: individual: 1H0419-577en
dc.subjectquasars: absorption linesen
dc.subjectquasarsen
dc.subjectemission linesen
dc.subjectquasars: generalen
dc.subjectX-rays: galaxiesen
dc.subjectactive galactic nucleien
dc.subjectreflection grating spectrometeren
dc.subjectquasar outflow contributionen
dc.subjectphoton imaging cameraen
dc.subjectx-ray/uv campaignen
dc.subjectmultiwavelengthen
dc.subjectcampaignen
dc.subjectwarm absorberen
dc.subjectagn feedbacken
dc.subjectintrinsic absorptionen
dc.subjecthst/cosen
dc.subjectobservationsen
dc.subjectAstronomy & Astrophysicsen
dc.titleSimultaneous XMM-Newton and HST-COS observation of 1H0419-577 The absorbing and emitting ionized gasen
dc.typeArticle - Refereeden
dc.contributor.departmentPhysicsen
dc.identifier.urlhttp://www.aanda.org/articles/aa/pdf/2013/08/aa21416-13.pdfen
dc.date.accessed2013-12-05en
dc.title.serialAstronomy & Astrophysicsen
dc.identifier.doihttps://doi.org/10.1051/0004-6361/201321416en


Files in this item

Thumbnail

This item appears in the following Collection(s)

Show simple item record