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HerMES: SPIRE emission from radio-selected active galactic nuclei

Seymour, N. and Blain, A. and Bock, J. and Cooray, A. and Dowell, C. D. and Levenson, L. and Lu, N. and Nguyen, H. T. and Schulz, B. and Shupe, D. L. and Xu, C. K. and Zemcov, M. (2011) HerMES: SPIRE emission from radio-selected active galactic nuclei. Monthly Notices of the Royal Astronomical Society, 413 (3). pp. 1777-1786. ISSN 0035-8711. http://resolver.caltech.edu/CaltechAUTHORS:20110531-151240573

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Abstract

We examine the rest-frame far-infrared emission from powerful radio sources with 1.4-GHz luminosity densities of 25 ≤ log(L_(1.4)/W Hz^(−1)) ≤ 26.5 in the extragalactic Spitzer First Look Survey field. We combine Herschel/SPIRE flux densities with Spitzer/Infrared Array Camera and Multiband Imaging Photometer for Spitzer infrared data to obtain total (8-1000 µm) infrared luminosities for these radio sources. We separate our sources into a moderate, 0.4 < z < 0.9, and a high, 1.2 < z < 3.0, redshift sub-sample and we use Spitzer observations of a z < 0.1 3CRR sample as a local comparison. By comparison to numbers from the Square Kilometre Array (SKA) Simulated Skies, we find that our moderate-redshift sample is complete and our high-redshift sample is 14 per cent complete. We constrain the ranges of mean star formation rates (SFRs) to be 3.4–4.2, 18–41 and 80–581 M_⊙ yr^(−1) for the local, moderate- and high-redshift samples, respectively. Hence, we observe an increase in the mean SFR with increasing redshift which we can parametrize as ∼(1 + z)^Q, where Q = 4.2 ± 0.8. However, we observe no trends of mean SFR with radio luminosity within the moderate- or high-redshift bins. We estimate that radio-loud active galactic nuclei (AGN) in the high-redshift sample contribute 0.1–0.5 per cent to the total SFR density at that epoch. Hence, if all luminous starbursts host radio-loud AGN we infer a radio-loud phase duty cycle of 0.001–0.005.


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http://dx.doi.org/10.1111/j.1365-2966.2011.18253.xDOIUNSPECIFIED
Additional Information:© 2011 The Authors. Monthly Notices of the Royal Astronomical Society © 2011 RAS. Accepted 2010 December 21. Received 2010 December 21; in original form 2010 September 24. Article first published online: 7 Mar 2011. Herschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA. NS thanks Carlos De Breuck, Martin Hardcastle, Curtis Saxton and Clive Tadhunter for useful discussions. 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 (UK) and NASA (USA). The data presented in this paper will be released through the Herschel Database in Marseille HeDaM hedam.oamp.fr/HerMES).
Group:TAPIR
Funders:
Funding AgencyGrant Number
CSA (Canada) UNSPECIFIED
NAOC (China) UNSPECIFIED
CEA (France)UNSPECIFIED
CNES (France) UNSPECIFIED
CNRS (France)UNSPECIFIED
ASI (Italy) UNSPECIFIED
MCINN (Spain)UNSPECIFIED
SNSB (Sweden) UNSPECIFIED
STFC (UK) UNSPECIFIED
NASAUNSPECIFIED
Subject Keywords: galaxies: active; infrared: galaxies; radio continuum: galaxies
Record Number:CaltechAUTHORS:20110531-151240573
Persistent URL:http://resolver.caltech.edu/CaltechAUTHORS:20110531-151240573
Official Citation:HerMES: SPIRE emission from radio-selected active galactic nuclei (pages 1777–1786) N. Seymour, M. Symeonidis, M. J. Page, A. Amblard, V. Arumugam, H. Aussel, A. Blain, J. Bock, A. Boselli, V. Buat, N. Castro-Rodríguez, A. Cava, P. Chanial, D. L. Clements, A. Conley, L. Conversi, A. Cooray, C. D. Dowell, E. Dwek, S. Eales, D. Elbaz, A. Franceschini, J. Glenn, E. A. González Solares, M. Griffin, E. Hatziminaoglou, E. Ibar, K. Isaak, R. J. Ivison, G. Lagache, L. Levenson, N. Lu, S. Madden, B. Maffei, G. Mainetti, L. Marchetti, H. T. Nguyen, B. O’Halloran, S. J. Oliver, A. Omont, P. Panuzzo, A. Papageorgiou, C. P. Pearson, I. Pérez-Fournon, M. Pohlen, J. I. Rawlings, D. Rizzo, I. G. Roseboom, M. Rowan-Robinson, B. Schulz, Douglas Scott, D. L. Shupe, A. J. Smith, J. A. Stevens, M. Trichas, K. E. Tugwell, M. Vaccari, I. Valtchanov, L. Vigroux, L. Wang, G. Wright, C. K. Xu and M. Zemcov Article first published online: 7 MAR 2011 | DOI: 10.1111/j.1365-2966.2011.18253.x
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:23845
Collection:CaltechAUTHORS
Deposited By: Ruth Sustaita
Deposited On:31 May 2011 23:00
Last Modified:23 Dec 2013 23:10

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