The Deep SPIRE HerMES Survey: spectral energy distributions and their astrophysical indications at high redshift

Creators: Brisbin, D.; Blain, A.; Bock, J. J.; Cooray, A.; Dowell, C. D.; Levenson, L.; Lu, N.; Nguyen, H. T.; Schulz, B.; Shupe, D. L.; Xu, C. K.; Zemcov, M.

Abstract

The Spectral and Photometric Imaging Receiver on-board Herschel has been carrying out deep extragalactic surveys, one of the aims of which is to establish spectral energy distributions of individual galaxies spanning the infrared/submillimetre (IR/SMM) wavelength region. We report observations of the IR/SMM emission from the Lockman North field and Great Observatories Origins Deep Survey Field-North. Because galaxy images in the wavelength range covered by Herschel generally represent a blend with contributions from neighbouring galaxies, we present sets of galaxies in each field, especially free of blending at 250, 350 and 500 μm. We identify the cumulative emission of these galaxies and the fraction of the FIR cosmic background radiation they contribute. Our surveys reveal a number of highly luminous galaxies at redshift z ≲ 3 and a novel relationship between IR and visible emission that shows a dependence on luminosity and redshift.

Additional Information

© 2010 The Authors. Journal compilation © 2010 RAS. Accepted 2010 September 3. Received 2010 September 2; in original form 2010 June 11. Article first published online: 25 Oct. 2010. Herschel is an ESA space observatory with science instruments provided by the European-led Principal Investigator consortia and with important participation from the NASA. This work is based in part on observations made with Herschel, a European Space Agency Cornerstone Mission with significant participation by the NASA. Support for this work was provided by the NASA through an award issued by JPL/Caltech. The SPIRE has been developed by a consortium of institutes led by Cardiff University (UK) and including Univ. Lethbridge (Canada); NAOC(China); CEA, OAMP(France); IFSI, Univ. Padua (Italy); IAC (Spain); Stockholm Observatory (Sweden); Imperial College London, RAL, UCL-MSSL, UKATC, Univ. Sussex (UK); and Caltech/JPL, IPAC, 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). We thank the referee of this paper, Stephen J. Messenger, for his incisive comments and helpful recommendations.

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