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Published November 1, 2015 | Published
Journal Article Open

Radio Jet Feedback and Star Formation in Heavily Obscured, Hyperluminous Quasars at Redshifts ~ 0.5–3. I. ALMA Observations


We present Atacama Large Millimeter/submillimeter Array (ALMA) 870 μm (345 GHz) data for 49 high-redshift (0.47 < z < 2.85), luminous 11.7 < log (L_(bol/L_⊙) < 14.2) radio-powerful active galactic nuclei (AGNs), obtained to constrain cool dust emission from starbursts concurrent with highly obscured radiative-mode black hole (BH) accretion in massive galaxies that possess a small radio jet. The sample was selected from the Wide-field Infrared Survey Explorer with extremely steep (red) mid-infrared colors and with compact radio emission from NVSS/FIRST. Twenty-six sources are detected at 870 μm, and we find that the sample has large mid- to far-infrared luminosity ratios, consistent with a dominant and highly obscured quasar. The rest-frame 3 GHz radio powers are 24.7 < log (P_(3.0 GHz)/W Hz^(-1)) and all sources are radio-intermediate or radio-loud. BH mass estimates are 7.7 < log(M_(BH)/M_⊙) < 10.2. The rest-frame 1–5 μm spectral energy distributions are very similar to the "Hot DOGs" (hot dust-obscured galaxies), and steeper (redder) than almost any other known extragalactic sources. ISM masses estimated for the ALMA-detected sources are 9.9 < log (M_(ISM)/M_⊙) < 11.75 assuming a dust temperature of 30 K. The cool dust emission is consistent with star formation rates reaching several thousand M_⊙ yr^(−1), depending on the assumed dust temperature, but we cannot rule out the alternative that the AGN powers all the emission in some cases. Our best constrained source has radiative transfer solutions with approximately equal contributions from an obscured AGN and a young (10–15 Myr) compact starburst.

Additional Information

© 2015. The American Astronomical Society. Received 2015 April 7; accepted 2015 August 28; published 2015 October 27. This paper makes use of the following ALMA data: ADS/JAO.ALMA#2011.0.00397.S. ALMA is a partnership of ESO (representing its member states), NSF (USA), and NINS (Japan), together with NRC (Canada), NSC and ASIAA (Taiwan), and KASI (Republic of Korea), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO, and NAOJ. This publication makes use of data products from the Wide-field Infrared Survey Explorer, which is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory/California Institute of Technology, funded by the National Aeronautics and Space Administration. This work is based on observations made with the Caltech Submillimeter Observatory, which is operated by the California Institute of Technology under funding from the National Science Foundation, contract AST 90-15755. This paper uses data from SDSS (DR 8). Funding for SDSS-III has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, and the U.S. Department of Energy Office of Science. The SDSS-III web site is http://www.sdss3.org/. RJA was supported by Gemini-CONICYT grant number 32120009. We thank the anonymous referee for comments that helped improve the paper. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. Facilities: WISE - Wide-field Infrared Survey Explorer, VLA - Very Large Array, ALMA - Atacama Large Millimeter Array, CTIO (SOAR–Goodman) - , Palomar 200 inch - , VLT - , Herschel - European Space Agency's Herschel space observatory, CSO - Caltech Submillimeter Observatory, Magellan - .

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