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Determining the zero-point calibration for AGN black hole mass estimates

Published online by Cambridge University Press:  24 November 2004

Christopher A. Onken ,
Laura Ferrarese ,
David Merritt ,
Bradley M. Peterson ,
Richard W. Pogge ,
Marianne Vestergaard  and
Amri Wandel
Christopher A. Onken
Affiliation:
Department of Astronomy, The Ohio State University, 140 West 18th Avenue, Columbus, OH 43210; [email protected], [email protected], [email protected]
Laura Ferrarese
Affiliation:
Department of Physics and Astronomy, Rutgers University, 136 Frelinghuysen Road, Piscataway, NJ 08854; [email protected]
David Merritt
Affiliation:
Department of Physics and Astronomy, Rutgers University, 136 Frelinghuysen Road, Piscataway, NJ 08854; [email protected] Current address: Department of Physics, Rochester Institute of Technology, 84 Lomb Memorial Drive, Rochester, NY 14623; [email protected]
Bradley M. Peterson
Affiliation:
Department of Astronomy, The Ohio State University, 140 West 18th Avenue, Columbus, OH 43210; [email protected], [email protected], [email protected]
Richard W. Pogge
Affiliation:
Department of Astronomy, The Ohio State University, 140 West 18th Avenue, Columbus, OH 43210; [email protected], [email protected], [email protected]
Marianne Vestergaard
Affiliation:
Department of Astronomy, The Ohio State University, 140 West 18th Avenue, Columbus, OH 43210; [email protected], [email protected], [email protected] Current address: Steward Observatory, University of Arizona, 933 North Cherry Avenue, Tucson, AZ 85721; [email protected]
Amri Wandel
Affiliation:
Racah Institute, Hebrew University, Jerusalem 91904, Israel; [email protected]
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Abstract

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By fitting to the quiescent galaxy MBH−σ∗ relation, we calculate the average shift required to scale reverberation-mapped AGN masses to the same zero-point. We use reanalyzed virial products (rV2/G) and both new and published velocity dispersions to find the offset in the AGN calibration. This scaling factor, 〈f〉, accounts for the detailed dynamics and geometry of the broad-line region (BLR). Finally, we confirm the rough correlation between σ∗ and FWHM([O III]) for these 16 AGNs.To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

Type
POSTERS
Information
Proceedings of the International Astronomical Union , Volume 2004 , Issue IAUS222 , March 2004 , pp. 109 - 110
Copyright
© 2004 International Astronomical Union