Mostrar registro simples

dc.contributor.authorKomossa, S.pt_BR
dc.contributor.authorXu, D.pt_BR
dc.contributor.authorZhou, H.pt_BR
dc.contributor.authorStorchi-Bergmann, Thaisapt_BR
dc.contributor.authorBinette, Lucpt_BR
dc.date.accessioned2015-01-15T02:15:12Zpt_BR
dc.date.issued2008pt_BR
dc.identifier.issn0004-637Xpt_BR
dc.identifier.urihttp://hdl.handle.net/10183/108977pt_BR
dc.description.abstractWe have studied the properties of Seyfert galaxies with high [O III] λ5007 blueshifts (‘‘blue outliers’’), originally identified because of their strong deviation from the MBH-σ relation of normal, narrow-line Seyfert 1 (NLS1) and broad-line Seyfert 1 (BLS1) galaxies. These blue outliers turn out to be important test beds for models of the narrowline region (NLR), for mechanisms of driving large-scale outflows, for links between NLS1 galaxies and radio galaxies, and for orientation-dependent NLS1 models.We report the detection of a strong correlation of line blueshift with ionization potential in each galaxy, including the measurement of coronal lines with radial velocities up to 500Y1000 km s-ˡ, and we confirm a strong correlation between [O III] blueshift and line width.All [O III] blue outliers have narrow widths of their broad Balmer lines and high Eddington ratios. While the presence of nonshifted lowionization lines signifies the presence of a classical outer quiescent NLR in blue outliers, we also report the absence of any second, nonblueshifted [O iii] component from a classical inner NLR. These results place tight constraints on NLR models.We favor a scenario in which the NLR clouds are entrained in a decelerating wind, which explains the strong stratification and the absence of a zero-blueshift inner NLR of blue outliers. The origin of the wind remains speculative at this time (collimated radio plasma, thermal winds, or radiatively accelerated clouds). It is perhaps linked to the high Eddington ratios of blue outliers. Similar, less powerful winds could be present in all Seyfert galaxies, but would generally only affect the coronal line region (CLR), or level off even before reaching the CLR. Similarities between blue outliers in NLS1 galaxies and (compact) radio sources are briefly discussed.en
dc.format.mimetypeapplication/pdf
dc.language.isoengpt_BR
dc.relation.ispartofThe astrophysical journal. Chicago. Vol. 680, no. 2, pt. 1 (June 2008), p. 926-938pt_BR
dc.rightsOpen Accessen
dc.subjectGalaxies: activeen
dc.subjectGalaxias seyfertpt_BR
dc.subjectGalaxies: evolutionen
dc.subjectGaláxias ativaspt_BR
dc.subjectRadiogalaxiaspt_BR
dc.subjectgalaxies: individual (SBS 0919+515, SDSS J115533.50+010730.4, RX J01354 0043, NGC 450-86, SDSS J032606.75+011429.9, IRAS 11598 0112, SDSS J171828.99+573422.3, PG 1244+026, RX J09132+3658)en
dc.subjectQuasarspt_BR
dc.subjectGalaxies: Seyferten
dc.subjectQuasars: emission linesen
dc.titleOn the nature of Seyfert galaxies with high [O III] λ5007 blueshiftspt_BR
dc.typeArtigo de periódicopt_BR
dc.identifier.nrb000766104pt_BR
dc.type.originEstrangeiropt_BR


Thumbnail
   

Este item está licenciado na Creative Commons License

Mostrar registro simples