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dc.contributor.authorRodriguez-Pascual, P.M.pt_BR
dc.contributor.authorAlloin, Danielle Mariept_BR
dc.contributor.authorClavel, J.pt_BR
dc.contributor.authorCrenshaw, Daniel Michaelpt_BR
dc.contributor.authorHorne, Keithpt_BR
dc.contributor.authorKriss, Gerard A.pt_BR
dc.contributor.authorKrolik, J.H.pt_BR
dc.contributor.authorMalkan, M.A.pt_BR
dc.contributor.authorNetzer, Hagaipt_BR
dc.contributor.authorO'Brien, P.T.pt_BR
dc.contributor.authorPeterson, Bradley M.pt_BR
dc.contributor.authorReichert, G.A.pt_BR
dc.contributor.authorWansteker, W.pt_BR
dc.contributor.authorAlexander, T.pt_BR
dc.contributor.authorBarr, P.pt_BR
dc.contributor.authorBlandford, R.D.pt_BR
dc.contributor.authorBregman, J.N.pt_BR
dc.contributor.authorCarone, T.E.pt_BR
dc.contributor.authorClements, S.pt_BR
dc.contributor.authorCourvoisier, T.-J.pt_BR
dc.contributor.authorDe Robertis, M.M.pt_BR
dc.contributor.authorDietrich, Matthiaspt_BR
dc.contributor.authorDottori, Horacio Albertopt_BR
dc.contributor.authorEdelson, Rick A.pt_BR
dc.contributor.authorFilippenko, Alexei V.pt_BR
dc.contributor.authorGaskell, C.M.pt_BR
dc.contributor.authorHuchra, John P.pt_BR
dc.contributor.authorHutchings, John B.pt_BR
dc.contributor.authorKollatschny, W.pt_BR
dc.contributor.authorKoratkar, A.P.pt_BR
dc.contributor.authorKorista, Kirk T.pt_BR
dc.contributor.authorLaor, A.pt_BR
dc.contributor.authorMacalpine, G.M.pt_BR
dc.contributor.authorMartin, P.G.pt_BR
dc.contributor.authorMaoz, D.pt_BR
dc.contributor.authorMccollum, B.pt_BR
dc.contributor.authorMorris, S.L.pt_BR
dc.contributor.authorPerola, G.C.pt_BR
dc.contributor.authorPogge, Richard Williampt_BR
dc.contributor.authorPtak, R.L.pt_BR
dc.contributor.authorRecondo-Gonzalez, M.C.pt_BR
dc.contributor.authorRodríguez Espinosa, Jose Miguelpt_BR
dc.contributor.authorRokaki, E.L.pt_BR
dc.contributor.authorSantos-Lleo, M.pt_BR
dc.contributor.authorSekiguchi, Kazuhiropt_BR
dc.contributor.authorShull, John Michaelpt_BR
dc.contributor.authorSnijders, M.A.J.pt_BR
dc.contributor.authorSparke, L.S.pt_BR
dc.contributor.authorStirpe, Giovanna M.pt_BR
dc.contributor.authorStoner, R.E.pt_BR
dc.contributor.authorSun, W.-H.pt_BR
dc.contributor.authorWagner, S.J.pt_BR
dc.contributor.authorWanders, I.pt_BR
dc.contributor.authorWilkes, B.J.pt_BR
dc.contributor.authorWinge, Claudiapt_BR
dc.contributor.authorZheng, W.pt_BR
dc.date.accessioned2015-01-20T02:15:11Zpt_BR
dc.date.issued1997pt_BR
dc.identifier.issn0067-0049pt_BR
dc.identifier.urihttp://hdl.handle.net/10183/109046pt_BR
dc.description.abstractAn 8 month monitoring campaign on the Seyfert 1 galaxy Fairall 9 has been conducted with the International Ultraviolet Explorer in an attempt to obtain reliable estimates of continuum-continuum and continuumÈemission-line delays for a high-luminosity active galactic nucleus (AGN). While the results of this campaign are more ambiguous than those of previous monitoring campaigns on lower luminosity sources, we Ðnd general agreement with the earlier results : (1) there is no measurable lag between ultraviolet continuum bands, and (2) the measured emission-line time lags are very short. It is especially notable that the Lyα + N V emission-line lag is about 1 order of magnitude smaller than determined from a previous campaign by Clavel, Wamsteker, & Glass (1989) when Fairall 9 was in a more luminous state. In other well-monitored sources, speciÐcally NGC 5548 and NGC 3783, the highest ionization lines are found to respond to continuum variations more rapidly than the lower ionization lines, which suggests a radially ionization-stratified broad-line region. In this case, the results are less certain, since none of the emission-line lags are very well determined. The best-determined emission line lag is Lyα + N V, for which we find that the centroid of the continuum—emission-line crosscorrelation function is tcent ≈14—20 days. We measure a lag tcent<~4 days for He II λ1640; this result is consistent with the ionization-stratification pattern seen in lower luminosity sources, but the relatively large uncertainties in the emission-line lags measured here cannot rule out similar lags for Lyα + N V and He II λ1640 at a high level of significance. We are unable to determine a reliable lag for C IV λ1550, but we note that the profiles of the variable parts of Lyα and C IV λ1550 are not the same, which does not support the hypothesis that the strongest variations in these two lines arise in the same region.en
dc.format.mimetypeapplication/pdf
dc.language.isoengpt_BR
dc.relation.ispartofThe Astrophysical journal. Supplement series. Chicago. Vol. 110, no. 1 (May 1997), p. 9-20pt_BR
dc.rightsOpen Accessen
dc.subjectAstronomia ultravioletapt_BR
dc.subjectGalaxies : activeen
dc.subjectEspectros astronômicospt_BR
dc.subjectGalaxies : individual (Fairall 9)en
dc.subjectNucleo galaticopt_BR
dc.subjectGalaxies : seyferten
dc.subjectUltraviolet : galaxiesen
dc.subjectGalaxias seyfertpt_BR
dc.titleSteps toward determination of the size and structure of the broad-line region in active galactic nuclei. IX. Ultraviolet observations of Fairall 9pt_BR
dc.typeArtigo de periódicopt_BR
dc.identifier.nrb000192549pt_BR
dc.type.originEstrangeiropt_BR


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