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Title:
Properties of Active Galaxies Deduced from H I Observations
Authors:
Ho, Luis C.; Darling, Jeremy; Greene, Jenny E.
Affiliation:
AA(The Observatories of the Carnegie Institution of Washington, 813 Santa Barbara Street, Pasadena, CA 91101.), AB(Center for Astrophysics and Space Astronomy, Department of Astrophysical and Planetary Sciences, University of Colorado, 389 UCB, Boulder, CO 80309-0389.), AC(Princeton Observatory, Peyton Hall, Princeton University, Princeton, NJ 08544-1001.; Hubble Fellow and Carnegie-Princeton Fellow.)
Publication:
The Astrophysical Journal, Volume 681, Issue 1, pp. 128-140. (ApJ Homepage)
Publication Date:
07/2008
Origin:
UCP
ApJ Keywords:
Galaxies: Active, Galaxies: Bulges, Galaxies: ISM, Galaxies: Kinematics and Dynamics, Galaxies: Nuclei, Galaxies: Seyfert
DOI:
10.1086/588207
Bibliographic Code:
2008ApJ...681..128H

Abstract

We have completed a new survey for H I emission for a large, well-defined sample of 154 nearby (z<~0.1) galaxies with type 1 (broad-line) active galactic nuclei (AGNs). We make use of the extensive database of H I and optical parameters, presented in a companion paper, to perform a comprehensive appraisal of the cold gas content in active galaxies and to seek new strategies to investigate the global properties of the host galaxies and their relationship to their central black holes. After excluding objects with kinematically anomalous line profiles, which occur with high frequency in the sample, we show that the black hole mass obeys a strong, roughly linear relation with the host galaxy's dynamical mass, calculated by combining the H I line width and the optical size of the galaxy. Black hole mass follows a looser, though still highly significant, correlation with the maximum rotation velocity of the galaxy, as expected from the known scaling between rotation velocity and central velocity dispersion. Neither of these H I-based correlations is as tight as the more familiar relations between black hole mass and bulge luminosity or velocity dispersion, but they offer the advantage of being insensitive to the glare of the nucleus and therefore are promising new tools for probing the host galaxies of both nearby and distant AGNs. We present evidence for substantial ongoing black hole growth in the most actively accreting AGNs. In these nearby systems, black hole growth appears to be delayed with respect to the assembly of the host galaxy but otherwise has left no detectable perturbation to its mass-to-light ratio, as judged from the Tully-Fisher relation, or its global gas content. The host galaxies of type 1 AGNs, including those luminous enough to qualify as quasars, are generally gas-rich systems, possessing a cold interstellar medium reservoir at least as abundant as that in inactive galaxies of the same morphological type. This calls into question current implementations of AGN feedback in models of galaxy formation that predict strong cold gas depletion in unobscured AGNs.
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