Show simple item record

dc.contributor.authorAlonso-Herrero, Almudena
dc.contributor.authorQuillen, Alice C.
dc.contributor.authorRieke, George H.
dc.contributor.authorIvanov, Valentin D.
dc.contributor.authorEfstathiou, Andreas
dc.date.accessioned2018-10-30T13:34:22Z
dc.date.available2018-10-30T13:34:22Z
dc.date.issued2003-07-01
dc.identifierSCOPUS_ID:0141863390
dc.identifier.issn00046256
dc.identifier.urihttps://www.scopus.com/inward/record.uri?partnerID=HzOxMe3b&scp=0141863390&origin=inward
dc.identifier.urihttps://repo.euc.ac.cy/handle/123456789/621
dc.description.abstractWe present nuclear spectral energy distributions (SEDs) in the range 0. 4-16 μm for an expanded CfA sample of Seyfert galaxies. The spectral indexes (fν α ν-αIR) from 1 to 16 μm range from αIR ∼ 0.9 to 3.8. The shapes of the spectra are correlated with Seyfert type in the sense that steeper nuclear SEDs (νf ν increasing with increasing wavelength) tend to be found in Seyfert 2's, and flatter SEDs (νfν is constant) in Seyfert 1-1.5's. The galaxies optically classified as Seyferts 1.8's and 1.9's display values of αIR as in type 1 objects, or values intermediate between those of Seyfert 1's and Seyfert 2's. The intermediate SEDs of many Seyfert 1.81.9's may be consistent with the presence of a pure Seyfert 1 viewed through a moderate amount (AV ≲ 5 mag) of foreground galaxy extinction. We find, however, that between 10% and 20% of galaxies with broad optical line components have steep infrared SEDs. Torus models usually adopt high equatorial opacities to reproduce the infrared properties of Seyfert 1's and 2's, resulting in a dichotomy of infrared SEDs (flat for type 1's, and steep for type 2's). Such a dichotomy, however, is not observed in our sample. The wide range of spectral indexes observed in the type 2 objects, the lack of extremely steep SEDs, and the large numbers of objects with intermediate spectral indexes cannot be reconciled with predictions from existing optically thick torus models. We discuss possible modifications to improve torus models, including low optical depth tori, clumpy dusty tori, and high optical depth tori with an extended optically thin component.
dc.relation.ispartofAstronomical Journal
dc.titleSpectral energy distributions of Seyfert nuclei
elsevier.identifier.doi10.1086/375545
elsevier.identifier.eid2-s2.0-0141863390
elsevier.identifier.scopusidSCOPUS_ID:0141863390
elsevier.volume126
elsevier.issue.identifier1 1771
elsevier.coverdate2003-07-01
elsevier.coverdisplaydateJuly 2003
elsevier.openaccess1
elsevier.openaccessflagtrue
elsevier.aggregationtypeJournal


Files in this item

FilesSizeFormatView

There are no files associated with this item.

This item appears in the following Collection(s)

Show simple item record