Extending virial black hole mass estimates to low-luminosity or obscured AGN: the cases of NGC 4395 and MCG -01-24-012
Date Issued
2015
Author(s)
La Franca, F.
•
•
Ricci, F.
•
Sani, E.
•
Brusa, M.
•
Maiolino, R.
•
Bianchi, S.
•
•
•
•
Vignali, C.
Description
We thank the referee for her/his very useful comments which improved the manuscript. Based on observations made with ESO telescopes at the Paranal Observatory and the Large Binocular Telescope (LBT) at Mt. Graham, Arizona. The LBT is an international collaboration among institutions in the United States, Italy, and Germany. LBT Corporation partners are: The University of Arizona on behalf of the Arizona university system; Istituto Nazionale di Astrofisica, Italy; LBT Beteiligungsgesellschaft, Germany, representing the Max-Planck Society, the Astrophysical Institute Potsdam, and Heidelberg University; The Ohio State University; and The Research Corporation, on behalf of The University of Notre Dame, University of Minnesota, and University of Virginia. We thank for the very efficient service observing mode operation management at LBT and the ESO staff at Paranal and Garching for their support during the preparation and execution of the observations. MB acknowledges support from the FP7 Career Integration Grant ‘eEASy’ (CIG 321913). We acknowledge funding from PRIN-MIUR 2010 award 2010NHBSBE and from PRIN-INAF 2011 ‘BH growth and AGN feedback through the cosmic time’.
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.
Volume
449
Issue
2
Start page
1526
Issn Identifier
0035-8711
Ads BibCode
2015MNRAS.449.1526L
Rights
open.access
File(s)![Thumbnail Image]()
![Thumbnail Image]()
Loading...
Name
LaFranca_1502.07234.pdf
Description
preprint
Size
428.73 KB
Format
Adobe PDF
Checksum (MD5)
b0e28adcc7d86c73006411aa3ff6ace2
Loading...
Name
LaFranca_stv368.pdf
Description
Pdf editoriale
Size
564.51 KB
Format
Adobe PDF
Checksum (MD5)
e174bb60443942ef92662bf55a688ce6