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A Deep Hubble Space Telescope H-Band Imaging Survey of Massive Gas-Rich Mergers. II. The QUEST QSOs

Veilleux, S. and Kim, D. C. and Rupke, D. S. N. and Peng, C. Y. and Tacconi, L. J. and Genzel, R. and Lutz, D. and Sturm, E. and Contursi, A. and Schweitzer, M. and Dasyra, K. M. and Ho, L. C. and Sanders, D. B. and Burkert, A. (2009) A Deep Hubble Space Telescope H-Band Imaging Survey of Massive Gas-Rich Mergers. II. The QUEST QSOs. Astrophysical Journal, 701 (1). pp. 587-606. ISSN 0004-637X. https://resolver.caltech.edu/CaltechAUTHORS:20090811-091437615

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Abstract

We report the results from a deep Hubble Space Telescope (HST) NICMOS H-band imaging survey of 28 z < 0.3 QSOs from the Palomar-Green (PG) sample. This program is part of QUEST (Quasar/ULIRG Evolution Study) and complements a similar set of data on 26 highly nucleated ULIRGs presented in Paper I. Our analysis indicates that the fraction of QSOs with elliptical hosts is higher among QSOs with undetected far-infrared (FIR) emission, small infrared excess (L_IR/L_B < 10), and luminous hosts. The hosts of FIR-faint QSOs show a tendency to have less pronounced merger-induced morphological anomalies and larger QSO-to-host luminosity ratios on average than the hosts of FIR-bright QSOs, consistent with late-merger evolution from FIR-bright to FIR-faint QSOs. The spheroid sizes (~ 0.3-5.5 kpc) and total host luminosities (~ 0.6-7.2 L*_H ) of the radio-quiet PG QSOs in our sample are statistically indistinguishable from the ULIRG hosts presented in Paper I, while those of radio-loud PG QSOs are systematically larger and more luminous. ULIRGs and PG QSOs with elliptical hosts fall near, but not exactly on, the fundamental plane of inactive spheroids. We confirm the systematic trend noted in Paper I for objects with small (~<2 kpc) spheroids to be up to ~ 1 mag brighter than inactive spheroids. The host colors and wavelength dependence of their sizes support the idea that these deviations are at least in part due to non-nuclear star formation. However, the amplitudes of these deviations depend mainly on host sizes, and possibly on infrared excess, but not on merger phase, QSO-to-host luminosity ratio, optical spectral type, active galactic nucleus fractional contribution to the bolometric luminosity, or host R – H color. Taken at face value (i.e., no correction for extinction or the presence of a young stellar population), the H-band spheroid-host luminosities imply black hole masses ~ (5-200) × 10^7 M and sub-Eddington mass accretion rates for both QSOs and ULIRGs. These results are compared with published black hole mass estimates derived from other methods.


Item Type:Article
Related URLs:
URLURL TypeDescription
http://dx.doi.org/10.1088/0004-637X/701/1/587DOIArticle
http://www.iop.org/EJ/abstract/0004-637X/701/1/587PublisherArticle
ORCID:
AuthorORCID
Veilleux, S.0000-0002-3158-6820
Tacconi, L. J.0000-0002-1485-9401
Genzel, R.0000-0002-2767-9653
Lutz, D.0000-0003-0291-9582
Ho, L. C.0000-0001-6947-5846
Sanders, D. B.0000-0002-1233-9998
Additional Information:© 2009. The American Astronomical Society. Received 2009 March 6; accepted 2009 June 15; published 2009 July 24. Print publication: Issue 1 (2009 August 10). Based on observations with the NASA/ESA Hubble Space Telescope, obtained at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract no. NAS5-26555. S.V., D.C.K., and D.S.N.R. were supported in part by NASA through grant HST-GO-10906.01-A. S.V. acknowledges support from a Senior Award from the Alexander von Humboldt Foundation and thanks the host institution, MPE Garching, where some of this work was performed. C.Y.P. is grateful to Space Telescope Science Institute for support through the Institute Fellowship program and to the National Research Council of Canada through the Plaskett Fellowship program at the Herzberg Institute of Astrophysics. We thank R. Davies, K. Jahnke, and E. Bell for comments on an earlier version of the manuscript, and the anonymous referee for a thoughtful review. This work has made use of NASA's Astrophysics Data System Abstract Service and the NASA/IPAC Extragalactic Database (NED), which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration.
Group:Infrared Processing and Analysis Center (IPAC)
Funders:
Funding AgencyGrant Number
NASANAS5-26555
NASAHST-GO-10906.01-A
Alexander von Humboldt FoundationUNSPECIFIED
Max Planck SocietyUNSPECIFIED
Space Telescope Science InstituteUNSPECIFIED
National Research Council of CanadaUNSPECIFIED
NASA/JPL/CaltechUNSPECIFIED
Subject Keywords:galaxies: active; galaxies: interactions; galaxies: Seyfert; galaxies: starburst; infrared: galaxies
Issue or Number:1
Record Number:CaltechAUTHORS:20090811-091437615
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20090811-091437615
Official Citation:A Deep Hubble Space Telescope H-Band Imaging Survey of Massive Gas-Rich Mergers. II. The QUEST QSOs S. Veilleux, D.-C. Kim, D. S. N. Rupke, C. Y. Peng, L. J. Tacconi, R. Genzel, D. Lutz, E. Sturm, A. Contursi, M. Schweitzer, K. M. Dasyra, L. C. Ho, D. B. Sanders, and A. Burkert 2009 ApJ 701 587-606 doi: 10.1088/0004-637X/701/1/587
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:14943
Collection:CaltechAUTHORS
Deposited By: George Porter
Deposited On:02 Sep 2009 19:54
Last Modified:09 Mar 2020 13:18

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