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Central Masses and Broad‐Line Region Sizes of Active Galactic Nuclei. II. A Homogeneous Analysis of a Large Reverberation‐Mapping Database

B. M. PetersonDepartment of Astronomy, The Ohio State University, 140 West 18th Avenue, Columbus, OH 43210Laura FerrareseDepartment of Physics and Astronomy, Rutgers University, 136 Frelinghuysen Road, Piscataway, NJ 08854Karoline M. GilbertCurrent address: University of California Observatories, Lick Observatory, University of California, Santa Cruz, CA 92064S. KaspiDepartment of Physics, Technion, Haifa 32000, IsraelMatthew A. MalkanDepartment of Physics and Astronomy, University of California, Los Angeles, CA 90095Dan MaozWise Observatory and School of Physics and Astronomy, Raymond and Beverly Sackler Faculty of Exact Sciences, Tel Aviv University, Tel Aviv 69978, IsraelDavid MerrittDepartment of Physics, Rochester Institute of Technology, 84 Lomb Memorial Drive, Rochester, NY 14623H. NetzerWise Observatory and School of Physics and Astronomy, Raymond and Beverly Sackler Faculty of Exact Sciences, Tel Aviv University, Tel Aviv 69978, IsraelChristopher A. OnkenDepartment of Astronomy, The Ohio State University, 140 West 18th Avenue, Columbus, OH 43210Richard W. PoggeDepartment of Astronomy, The Ohio State University, 140 West 18th Avenue, Columbus, OH 43210M. VestergaardSteward Observatory, University of Arizona, Tucson, AZ 85721Amri WandelRacah Institute of Physics, The Hebrew University, Jerusalem 91405, Israel

2004en

ABI

Annotatsiya

The masses and emission-line region sizes of AGNs can be measured by “reverberation-mapping ” techniques and we use these results to calibrate similar determinations made by photoionization models of the AGN line-emitting regions. Reverberation mapping uses the light travel-time delayed emission-line response to continuum variations to determine the size and kinematics of the emission-line region. We compile a sample of 17 Seyfert 1 galaxies and 2 quasars with reliable reverberation and spectroscopy data, twice the number available previously. The data provide strong evidence that the BLR size (as measured by the lag of the emission-line luminosity after changes in the continuum) and the emission-line width measure directly the central mass: the virial assumption is tested with long-term UV and optical monitoring data on NGC 5548. Two methods are used to estimate the distance of the broad emission-line region (BLR) from the ionizing source: the photoionization method (which is available for many AGNs but has large intrinsic uncertainties), and the reverberation method (which gives very reliable distances, but is available for only a

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DOI: 10.1086/423269

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