Please use this identifier to cite or link to this item:
http://hdl.handle.net/2307/391
DC Field | Value | Language |
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dc.contributor.author | Lamastra, Alessandra | - |
dc.contributor.author | Bianchi, Stefano | - |
dc.contributor.author | Matt, Giorgio | - |
dc.contributor.author | Perola, Giuseppe Cesare | - |
dc.contributor.author | Barcons, X. | - |
dc.contributor.author | Carrera, F. J. | - |
dc.date.accessioned | 2010-07-30T15:46:55Z | - |
dc.date.available | 2010-07-30T15:46:55Z | - |
dc.date.issued | 2009-09 | - |
dc.identifier.issn | 0004-6361 | - |
dc.identifier.uri | http://hdl.handle.net/2307/391 | - |
dc.description.abstract | Context. There have been recent claims that a significant fraction of type 2 AGN accrete close to or even above the Eddington limit. In type 2 AGN, the bolometric luminosity (L-b) is generally inferred from the [OIII] emission line luminosity (L-OIII). The key issue in estimating the bolometric luminosity in these AGN, is therefore to know the bolometric correction to be applied to L-OIII. A complication arises from the observed L-OIII being affected by extinction, most likely from dust within the narrow line region. The extinction-corrected [OIII] luminosity (L-OIII(c)) is a better estimator of the nuclear luminosity than L-OIII. However, only the bolometric correction to be applied to the uncorrected L-OIII has been evaluated so far. Aims. This paper is devoted to estimating the bolometric correction C-OIII = L-b/L-OIII(c) for deriving the Eddington ratios for the type 2 AGN in a sample of SDSS objects. Methods. We collected 61 sources from the literature with reliable estimates of both L-OIII(c) and X-ray luminosities (L-X). To estimate C-OIII, we combined the observed correlation between L-OIII(c) and L-Xwith the X-ray bolometric correction. Results. In contrast to previous studies, we found a linear correlation between L-OIII(c) and L-X. We estimated C-OIII using an earlier luminosity-dependent X-ray bolometric correction, and we found a mean value of C-OIII in the luminosity ranges log L-OIII = 38-40, 40-42, and 42-44 of 87, 142, and 454, respectively. We used it to calculate the Eddington ratio distribution of type 2 SDSS AGN at 0.3 < z < 0.4 and found that these sources are not accreting near their Eddington limit, contrary to previous claims. | en |
dc.language.iso | en | en |
dc.publisher | EDP Sciences | en |
dc.relation.ispartof | Astronomy & Astrophysics | en |
dc.rights | ESO | en |
dc.subject | ACTIVE GALACTIC NUCLEI | en |
dc.subject | DIGITAL-SKY-SURVEY | en |
dc.subject | BLACK-HOLE MASSES | en |
dc.subject | BROAD-LINE REGION | en |
dc.subject | X-RAY | en |
dc.subject | VELOCITY DISPERSION | en |
dc.subject | SEYFERT-GALAXIES | en |
dc.subject | EMISSION-LINE | en |
dc.subject | HOST GALAXIES | en |
dc.subject | QUASARS | en |
dc.title | The bolometric luminosity of type 2 AGN from extinction-corrected [OIII]: no evidence of Eddington-limited sources | en |
dc.type | Article | en |
dc.subject.miur | Settori Disciplinari MIUR::Scienze fisiche::ASTRONOMIA E ASTROFISICA | en |
dc.subject.miur | Scienze fisiche | - |
dc.subject.isicrui | Categorie ISI-CRUI::Scienze fisiche::Physics | en |
dc.subject.isicrui | Scienze fisiche | - |
dc.subject.anagraferoma3 | Scienze fisiche | en |
dc.relation.volumenumber | 504 | en |
dc.relation.pagenumber | 73-79 | en |
dc.identifier.url | http://arxiv.org/abs/0905.4439 | - |
dc.identifier.doi | 10.1051/0004-6361/200912023 | - |
dc.relation.issuenumber | 1 | en |
dc.description.romatrecurrent | Dipartimento di Fisica 'Edoardo Amaldi' | * |
item.languageiso639-1 | other | - |
item.fulltext | With Fulltext | - |
item.grantfulltext | open | - |
Appears in Collections: | A - Articolo su rivista X_Dipartimento di Fisica 'Edoardo Amaldi' |
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File | Description | Size | Format | |
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thebolometricluminosity.pdf | solo archivio | 167.52 kB | Adobe PDF | View/Open |
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