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dc.contributor.authorLamperti, Isabellapt_BR
dc.contributor.authorKoss, Michaelpt_BR
dc.contributor.authorTrakhtenbrot, Bennypt_BR
dc.contributor.authorSchawinski, Kevinpt_BR
dc.contributor.authorRicci, Claudiopt_BR
dc.contributor.authorOh, Kyuseokpt_BR
dc.contributor.authorLandt, Herminept_BR
dc.contributor.authorRiffel, Rogériopt_BR
dc.contributor.authorRodriguez-Ardila, Albertopt_BR
dc.contributor.authorGehrels, Neil C.pt_BR
dc.contributor.authorHarrison, Fiona Annept_BR
dc.contributor.authorMasetti, Nicolapt_BR
dc.contributor.authorMushotzky, Richardpt_BR
dc.contributor.authorTreister, Ezequielpt_BR
dc.contributor.authorUeda, Yoshihiropt_BR
dc.contributor.authorVeilleux, Sylvainpt_BR
dc.date.accessioned2017-06-20T02:33:27Zpt_BR
dc.date.issued2017pt_BR
dc.identifier.issn0035-8711pt_BR
dc.identifier.urihttp://hdl.handle.net/10183/159781pt_BR
dc.description.abstractWe provide a comprehensive census of the near-infrared (NIR, 0.8–2.4 μm) spectroscopic properties of 102 nearby (z < 0.075) active galactic nuclei (AGN), selected in the hard X-ray band (14–195 keV) from the Swift-Burst Alert Telescope survey.With the launch of the James Webb Space Telescope, this regime is of increasing importance for dusty and obscured AGN surveys. We measure black hole masses in 68 per cent (69/102) of the sample using broad emission lines (34/102) and/or the velocity dispersion of the Ca II triplet or the CO band-heads (46/102). We find that emission-line diagnostics in the NIR are ineffective at identifying bright, nearby AGN galaxies because [Fe II] 1.257 μm/Paβ and H2 2.12 μm/Brγ identify only 25 per cent (25/102) as AGN with significant overlap with star-forming galaxies and only 20 per cent of Seyfert 2 have detected coronal lines (6/30). We measure the coronal line emission in Seyfert 2 to be weaker than in Seyfert 1 of the same bolometric luminosity suggesting obscuration by the nuclear torus. We find that the correlation between the hard X-ray and the [Si VI] coronal line luminosity is significantly better than with the [OIII] λ5007 luminosity. Finally, we find 3/29 galaxies (10 per cent) that are optically classified as Seyfert 2 show broad emission lines in the NIR. These AGN have the lowest levels of obscuration among the Seyfert 2s in our sample (logNH < 22.43 cm−2), and all show signs of galaxy-scale interactions or mergers suggesting that the optical broad emission lines are obscured by host galaxy dust.en
dc.format.mimetypeapplication/pdfpt_BR
dc.language.isoengpt_BR
dc.relation.ispartofMonthly notices of the Royal Astronomical Society. Oxford. Vol. 467, no. 1 (May 2017), p. 540-572pt_BR
dc.rightsOpen Accessen
dc.subjectGaláxias ativaspt_BR
dc.subjectGalaxies activeen
dc.subjectQuasarspt_BR
dc.subjectQuasars emission linesen
dc.subjectQuasars generalen
dc.subjectGalaxias seyfertpt_BR
dc.subjectGalaxies seyferten
dc.subjectAstronomia infravermelhapt_BR
dc.subjectBuracos negrospt_BR
dc.subjectInfrared galaxiesen
dc.subjectX-rays galaxiesen
dc.titleBAT AGN Spectroscopic Survey -IV. : near-infrared coronal lines, hidden broad lines and correlation with hard X-ray emissionpt_BR
dc.typeArtigo de periódicopt_BR
dc.identifier.nrb001022448pt_BR
dc.type.originEstrangeiropt_BR


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