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Star formation rates in luminous quasars at 2 < z < 3

Harris, Kathryn and Farrah, Duncan and Schulz, Bernhard and Hatziminaoglou, Evanthia and Viero, Marco and Anderson, Nick and Béthermin, Matthieu and Chapman, Scott and Clements, David L. and Cooray, Asantha and Efstathiou, Andreas and Feltre, Anne and Hurley, Peter and Ibar, Eduardo and Lacy, Mark and Oliver, Sebastian and Page, Mathew J. and Pérez-Fournon, Ismael and Petty, Sara M. and Pitchford, Lura K. and Rigopoulou, Dimitra and Scott, Douglas and Symeonidis, Myrto and Vieira, Joaquin and Wang, Lingyu (2016) Star formation rates in luminous quasars at 2 < z < 3. Monthly Notices of the Royal Astronomical Society, 457 (4). pp. 4179-4194. ISSN 0035-8711. https://resolver.caltech.edu/CaltechAUTHORS:20160503-111306228

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Abstract

We investigate the relation between star formation rates (M_s) and AGN properties in optically selected type 1 quasars at 2 < z < 3 using data from Herschel and the SDSS. We find that M_s remains approximately constant with redshift, at 300 ± 100 M⊙ yr^(−1). Conversely, M_s increases with AGN luminosity, up to a maximum of ∼ 600 M⊙ yr^(−1), and with C IV FWHM. In context with previous results, this is consistent with a relation between M_s and black hole accretion rate (M_(bh)) existing in only parts of the z−M_s–M_(bh) plane, dependent on the free gas fraction, the trigger for activity, and the processes that may quench star formation. The relations between M_s and both AGN luminosity and C IV FWHM are consistent with star formation rates in quasars scaling with black hole mass, though we cannot rule out a separate relation with black hole accretion rate. Star formation rates are observed to decline with increasing C IV equivalent width. This decline can be partially explained via the Baldwin effect, but may have an additional contribution from one or more of three factors; M_i is not a linear tracer of L_(2500), the Baldwin effect changes form at high AGN luminosities, and high C IV EW values signpost a change in the relation between M_s and M_(bh). Finally, there is no strong relation between M_s and Eddington ratio, or the asymmetry of the C IV line. The former suggests that star formation rates do not scale with how efficiently the black hole is accreting, while the latter is consistent with C IV asymmetries arising from orientation effects.


Item Type:Article
Related URLs:
URLURL TypeDescription
http://dx.doi.org/10.1093/mnras/stw286DOIArticle
http://mnras.oxfordjournals.org/content/457/4/4179PublisherArticle
http://arxiv.org/abs/1602.02755arXivDiscussion Paper
http://mnras.oxfordjournals.org/content/457/4/4179/suppl/DC1PublisherSupporting Information
ORCID:
AuthorORCID
Farrah, Duncan0000-0003-1748-2010
Béthermin, Matthieu0000-0002-3915-2015
Clements, David L.0000-0002-9548-5033
Cooray, Asantha0000-0002-3892-0190
Efstathiou, Andreas0000-0002-2612-4840
Lacy, Mark0000-0002-3032-1783
Oliver, Sebastian0000-0001-7862-1032
Page, Mathew J.0000-0002-6689-6271
Petty, Sara M.0000-0003-0624-3276
Scott, Douglas0000-0002-6878-9840
Additional Information:© 2016 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. Accepted 2016 February 2; Received 2016 January 31; in original form 2015 October 8; First published online February 5, 2016. We thank the referee for a very helpful report. Herschel is an ESA space observatory with instruments provided by European-led Principal Investigator consortia and with participation from NASA. The Herschel spacecraft was designed, built, tested, and launched under a contract to ESA managed by the Herschel/Planck Project team by an industrial consortium under the overall responsibility of the prime contractor Thales Alenia Space (Cannes), and including Astrium (Friedrichshafen) responsible for the payload module and for system testing, Thales Alenia Space (Turin) responsible for the service module, and Astrium (Toulouse) responsible for the telescope, with in excess of a hundred subcontractors. SPIRE has been developed by a consortium of institutes led by Cardiff Univ. (UK) and including: Univ. Lethbridge (Canada); NAOC (China); CEA, LAM (France); IFSI, Univ. Padua (Italy); IAC (Spain); Stockholm Observatory (Sweden); Imperial College London, RAL, UCL-MSSL, UKATC, Univ. Sussex (UK); and Caltech, JPL, NHSC, Univ. Colorado (USA). This development has been supported by national funding agencies: CSA (Canada); NAOC (China); CEA, CNES, CNRS (France); ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC, UKSA (UK); and NASA (USA). 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. SDSS-III is managed by the Astrophysical Research Consortium for the Participating Institutions of the SDSS-III Collaboration including the University of Arizona, the Brazilian Participation Group, Brookhaven National Laboratory, Carnegie Mellon University, University of Florida, the French Participation Group, the German Participation Group, Harvard University, the Instituto de Astrofisica de Canarias, the Michigan State/Notre Dame/JINA Participation Group, Johns Hopkins University, Lawrence Berkeley National Laboratory, Max Planck Institute for Astrophysics, Max Planck Institute for Extraterrestrial Physics, New Mexico State University, New York University, Ohio State University, Pennsylvania State University, University of Portsmouth, Princeton University, the Spanish Participation Group, University of Tokyo, University of Utah, Vanderbilt University, University of Virginia, University of Washington, and Yale University. AF acknowledges support from the ERC via an Advanced Grant 321323-NEOGAL.
Group:Infrared Processing and Analysis Center (IPAC)
Funders:
Funding AgencyGrant Number
Canadian Space Agency (CSA)UNSPECIFIED
National Astronomical Observatories of ChinaUNSPECIFIED
Commissariat à l’Energie Atomique (CEA)UNSPECIFIED
Centre National d'Études Spatiales (CNES)UNSPECIFIED
Centre National de la Recherche Scientifique (CNRS)UNSPECIFIED
Agenzia Spaziale Italiana (ASI)UNSPECIFIED
Ministerio de Ciencia e Innovación (MCINN)UNSPECIFIED
Swedish National Space Board (SNSB)UNSPECIFIED
Science and Technology Facilities Council (STFC)UNSPECIFIED
United Kingdom Space Agency (UKSA)UNSPECIFIED
NASAUNSPECIFIED
Alfred P. Sloan FoundationUNSPECIFIED
Participating InstitutionsUNSPECIFIED
NSFUNSPECIFIED
Department of Energy (DOE)UNSPECIFIED
European Research Council (ERC)321323-NEOGAL
Issue or Number:4
Record Number:CaltechAUTHORS:20160503-111306228
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20160503-111306228
Official Citation:Kathryn Harris, Duncan Farrah, Bernhard Schulz, Evanthia Hatziminaoglou, Marco Viero, Nick Anderson, Matthieu Béthermin, Scott Chapman, David L. Clements, Asantha Cooray, Andreas Efstathiou, Anne Feltre, Peter Hurley, Eduardo Ibar, Mark Lacy, Sebastian Oliver, Mathew J. Page, Ismael Pérez-Fournon, Sara M. Petty, Lura K. Pitchford, Dimitra Rigopoulou, Douglas Scott, Myrto Symeonidis, Joaquin Vieira, and Lingyu Wang Star formation rates in luminous quasars at 2 < z < 3 MNRAS (April 21, 2016) Vol. 457 4179-4194 doi:10.1093/mnras/stw286 first published online February 5, 2016
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:66618
Collection:CaltechAUTHORS
Deposited By: Tony Diaz
Deposited On:04 May 2016 04:52
Last Modified:03 Oct 2019 09:58

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