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The Geometry of the Infrared and X-Ray Obscurer in a Dusty Hyperluminous Quasar

Farrah, Duncan and Baloković, Mislav and Stern, Daniel and Harris, Kathryn and Kunimoto, Michelle and Walton, Dominic J. and Alexander, David M. and Arévalo, Patricia and Ballantyne, David R. and Bauer, Franz E. and Boggs, Steven and Brandt, William N. and Brightman, Murray and Christensen, Finn and Clements, David L. and Craig, William and Fabian, Andrew and Hailey, Charles and Harrison, Fiona and Koss, Michael and Lansbury, George B. and Luo, Bin and Paine, Jennie and Petty, Sara and Pitchford, Kate and Ricci, Claudio and Zhang, William (2016) The Geometry of the Infrared and X-Ray Obscurer in a Dusty Hyperluminous Quasar. Astrophysical Journal, 831 (1). Art. No. 76. ISSN 0004-637X.

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We study the geometry of the active galactic nucleus (AGN) obscurer in IRAS 09104+4109, an IR-luminous, radio-intermediate FR-I source at z = 0.442, using infrared data from Spitzer and Herschel, X-ray data from NuSTAR, Swift, Suzaku, and Chandra, and an optical spectrum from Palomar. The infrared data imply a total rest-frame 1–1000 μm luminosity of 5.5 × 10^(46) erg s^(−1) and require both an AGN torus and a starburst model. The AGN torus has an anisotropy-corrected IR luminosity of 4.9 × 10^(46) erg s^(−1) and a viewing angle and half-opening angle both of approximately 36° from pole-on. The starburst has a star formation rate of (110 ± 34) M_⊙ yr^(−1) and an age of <50 Myr. These results are consistent with two epochs of luminous activity in IRAS 09104+4109: one approximately 150 Myr ago, and one ongoing. The X-ray data suggest a photon index of Γ ≃ 1.8 and a line-of-sight column density of N_H ≃ 5 × 10^(23) cm^(−2). This argues against a reflection-dominated hard X-ray spectrum, which would have implied a much higher N_H and luminosity. The X-ray and infrared data are consistent with a bolometric AGN luminosity of L(bol) ~ (0.5–2.5) × 10^(47) erg s^(−1). The X-ray and infrared data are further consistent with coaligned AGN obscurers in which the line of sight "skims" the torus. This is also consistent with the optical spectra, which show both coronal iron lines and broad lines in polarized but not direct light. Combining constraints from the X-ray, optical, and infrared data suggest that the AGN obscurer is within a vertical height of 20 pc, and a radius of 125 pc, of the nucleus.

Item Type:Article
Related URLs:
URLURL TypeDescription Paper
Farrah, Duncan0000-0003-1748-2010
Stern, Daniel0000-0003-2686-9241
Walton, Dominic J.0000-0001-5819-3552
Alexander, David M.0000-0002-5896-6313
Ballantyne, David R.0000-0001-8128-6976
Bauer, Franz E.0000-0002-8686-8737
Boggs, Steven0000-0001-9567-4224
Brandt, William N.0000-0002-0167-2453
Clements, David L.0000-0002-9548-5033
Harrison, Fiona0000-0003-2992-8024
Koss, Michael0000-0002-7998-9581
Lansbury, George B.0000-0002-5328-9827
Luo, Bin0000-0002-9036-0063
Ricci, Claudio0000-0001-5231-2645
Additional Information:© 2016. The American Astronomical Society. Received 2016 February 22; revised 2016 June 14; accepted 2016 June 14; published 2016 October 27. We thank the referee for a very helpful report. This work was supported under NASA Contract No. NNG08FD60C and made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software, and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). Herschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA. PACS has been developed by a consortium of institutes led by MPE (Germany) and including UVIE (Austria); KU Leuven, CSL, IMEC (Belgium); CEA, LAM (France); MPIA (Germany); INAF-IFSI/OAA/OAP/OAT, LENS, SISSA (Italy); and IAC (Spain). This development has been supported by the funding agencies BMVIT (Austria), ESA-PRODEX (Belgium), CEA/CNES (France), DLR (Germany), ASI/INAF (Italy), and CICYT/MCYT (Spain). This work is based in part on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. Part of this work is based on archival data, software, and online services provided by the ASDC. This research has made use of NASA's Astrophysics Data System. We acknowledge support from the NASA Earth and Space Science Fellowship Program grant NNX14AQ07H (M.B.), CONICYT-Chile grants Basal-CATA PFB-06/2007 (F.E.B., C.R.), FONDECYT Regular 1141218 (F.E.B., C.R.), "EMBIGGEN" Anillo ACT1101 (F.E.B., C.R.), and the Ministry of Economy, Development, and Tourism's Millennium Science Initiative through grant IC120009, awarded to The Millennium Institute of Astrophysics, MAS (F.E.B.). A.C.F. acknowledges ERC Advanced Grant Feedback 340442. Facilities: NuSTAR - The NuSTAR (Nuclear Spectroscopic Telescope Array) mission, Swift - , Suzaku - , Chandra - , Spitzer - , Herschel - , Palomar - .
Funding AgencyGrant Number
NASA Earth and Space Science FellowshipNNX14AQ07H
Comisión Nacional de Investigación Científica y Tecnológica (CONICYT)Basal-CATA PFB-06/2007
Fondo Nacional de Desarrollo Científico y Tecnológico (FONDECYT)1141218
Comisión Nacional de Investigación Científica y Tecnológica (CONICYT)Anillo ACT1101
Iniciativa Científica Milenio del Ministerio de Economía, Fomento y TurismoIC120009
European Research Council (ERC)340442
Subject Keywords:galaxies: evolution; galaxies: individual (IRAS 09104+4109) ; galaxies: Seyfert; galaxies: starburst; infrared: galaxies; X-rays: galaxies
Record Number:CaltechAUTHORS:20161027-143757170
Persistent URL:
Official Citation:Duncan Farrah et al 2016 ApJ 831 76
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:71561
Deposited By: George Porter
Deposited On:28 Oct 2016 16:38
Last Modified:30 Nov 2017 16:53

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