In the last decade, using single epoch (SE) virial based spectroscopic optical observations, it has been possible to measure the black hole (BH) mass on large type 1 active galactic nuclei (AGN) samples. However this kind of measurements cannot be applied on those obscured type 2 and/or low-luminosity AGN where the nuclear component does not dominate in the optical. We have derived new SE relationships, based on the full width at half-maximum and luminosity of the broad-line region component of the Paβ emission line and/or the hard X-ray luminosity in the 14-195 keV band, which have the prospect of better working with low luminosity or obscured AGN. The SE relationships have been calibrated in the 105-109 M⊙ mass range, using a sample of AGN, whose BH masses have been previously measured using reverberation mapping techniques. Our tightest relationship between the reverberation-based BH mass and the SE virial product has an intrinsic spread of 0.20 dex. Thanks to these SE relations, in agreement with previous estimates, we have measured a BH mass of M_BH = 1.7^{+1.3}_{-0.7} × 10^5 M⊙ for the low luminosity, type 1, AGN NGC 4395 (one of the smallest active galactic BH known). We also measured, for the first time, a BH mass of M_BH = 1.5^{+1.1}_{-0.6} × 10^7 M⊙ for the Seyfert 2 galaxy MCG -01-24-012.

LA FRANCA, F., Onori, F., Ricci, F., Sani, E., Brusa, M., Maiolino, R., et al. (2015). Extending virial black hole mass estimates to low-luminosity or obscured AGN: the cases of NGC 4395 and MCG-01-24-012. MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY, 449(2), 1526-1535 [10.1093/mnras/stv368].

Extending virial black hole mass estimates to low-luminosity or obscured AGN: the cases of NGC 4395 and MCG-01-24-012

F. La Franca,;Onori, F.;Ricci, F.;Brusa, M.;Maiolino, R.;Bianchi, S.;Fiore, F.;Vignali, C.;Marconi, A.
2015-01-01

Abstract

In the last decade, using single epoch (SE) virial based spectroscopic optical observations, it has been possible to measure the black hole (BH) mass on large type 1 active galactic nuclei (AGN) samples. However this kind of measurements cannot be applied on those obscured type 2 and/or low-luminosity AGN where the nuclear component does not dominate in the optical. We have derived new SE relationships, based on the full width at half-maximum and luminosity of the broad-line region component of the Paβ emission line and/or the hard X-ray luminosity in the 14-195 keV band, which have the prospect of better working with low luminosity or obscured AGN. The SE relationships have been calibrated in the 105-109 M⊙ mass range, using a sample of AGN, whose BH masses have been previously measured using reverberation mapping techniques. Our tightest relationship between the reverberation-based BH mass and the SE virial product has an intrinsic spread of 0.20 dex. Thanks to these SE relations, in agreement with previous estimates, we have measured a BH mass of M_BH = 1.7^{+1.3}_{-0.7} × 10^5 M⊙ for the low luminosity, type 1, AGN NGC 4395 (one of the smallest active galactic BH known). We also measured, for the first time, a BH mass of M_BH = 1.5^{+1.1}_{-0.6} × 10^7 M⊙ for the Seyfert 2 galaxy MCG -01-24-012.
LA FRANCA, F., Onori, F., Ricci, F., Sani, E., Brusa, M., Maiolino, R., et al. (2015). Extending virial black hole mass estimates to low-luminosity or obscured AGN: the cases of NGC 4395 and MCG-01-24-012. MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY, 449(2), 1526-1535 [10.1093/mnras/stv368].
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Utilizza questo identificativo per citare o creare un link a questo documento: https://hdl.handle.net/11590/282743
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