Please use this identifier to cite or link to this item: http://hdl.handle.net/2307/273
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dc.contributor.authorBianchi, Stefano-
dc.contributor.authorLa Franca, Fabio-
dc.contributor.authorMatt, Giorgio-
dc.contributor.authorGuainazzi, Matteo-
dc.contributor.authorJimenez Bailon, Elena-
dc.contributor.authorLonginotti, Anna Lia-
dc.contributor.authorNicastro, Fabrizio-
dc.contributor.authorPentericci, Laura-
dc.date.accessioned2010-07-08T10:16:16Z-
dc.date.available2010-07-08T10:16:16Z-
dc.date.issued2008-07-
dc.identifier.urihttp://hdl.handle.net/2307/273-
dc.description.abstractThe X-ray spectrum of NGC 7213 is known to present no evidence for Compton reflection, a unique result among bright Seyfert 1s. The observed neutral iron Kα line, therefore, cannot be associated with a Compton-thick material, like the disc or the torus, but is due to Compton-thin gas, with the broad-line region (BLR) as the most likely candidate. To check this hypothesis, a long Chandra High-Energy Transmission Grating observation, together with a quasi-simultaneous optical spectroscopic observation at the ESO NTT EMMI were performed. We found that the iron line is resolved with a full width at half-maximum (FWHM) = 2400+1100-600kms-1, in perfect agreement with the value measured for the broad component of the Hα, 2640+110-90kms-1. Therefore, NGC 7213 is the only Seyfert 1 galaxy whose iron Kα line is unambiguously produced in the BLR. We also confirmed the presence of two ionized iron lines and studied them in greater detail than before. The resonant line is the dominant component in the Fe XXV triplet, therefore suggesting an origin in collisionally ionized gas. If this is the case, the blueshift of around 1000kms-1 of the two ionized iron lines could be the first measure of the velocity of a starburst wind from its X-ray emission.en
dc.language.isoenen
dc.publisherWiley-Blackwellen
dc.relation.ispartofMonthly Notices of the Royal Astronomical Society: Lettersen
dc.subjectAstrofisicaen
dc.subjectgalassieen
dc.subjectAGNen
dc.titleA broad-line region origin for the iron Kα line in NGC 7213en
dc.typeArticleen
dc.subject.miurSettori Disciplinari MIUR::Scienze fisiche::ASTRONOMIA E ASTROFISICAen
dc.subject.isicruiCategorie ISI-CRUI::Scienze fisiche::Physicsen
dc.subject.isicruiCategorie ISI-CRUI::Scienze fisiche::Space Scienceen
dc.subject.isicruiCategorie ISI-CRUI::Scienze fisiche::Spectroscopy/Instrumentation/Analytical Sciencesen
dc.subject.anagraferoma3Scienze fisicheen
dc.relation.volumenumber389en
dc.relation.pagenumber52-56en
dc.identifier.urlhttp://www3.interscience.wiley.com/cgi-bin/fulltext/120847823/PDFSTART-
dc.identifier.doi10.1111/j.1745-3933.2008.00521.x-
dc.relation.issuenumber1en
item.languageiso639-1other-
item.fulltextWith Fulltext-
item.grantfulltextrestricted-
Appears in Collections:A - Articolo su rivista
X_Dipartimento di Fisica 'Edoardo Amaldi'
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