Clements, D. L. and Vaccari, M. and Babbedge, T. and Oliver, S. and Rowan-Robinson, M. and Davoodi, P. and Ivison, R. and Farrah, D. and Dunlop, J. and Shupe, Dave and Waddington, I. and Simpson, C. and Furusawa, H. and Serjeant, S. and Afonso-Luis, A. and Alexander, D. M. and Aretxaga, I. and Blain, A. and Borys, C. and Chapman, S. and Coppin, K. and Dunne, L. and Dye, S. and Eales, S. A. and Evans, T. and Fang, F. and Frayer, D. and Fox, M. and Gear, W. K. and Greve, T. R. and Halpern, M. and Hughes, D. H. and Jennes, T. and Lonsdale, C. J. and Mortier, A. M. and Page, M. J. and Pope, A. and Priddey, R. S. and Rawlings, S. and Savage, R. S. and Scott, D. and Scott, S. E. and Sekiguchi, K. and Smail, I. and Smith, H. E. and Stevens, J. A. and Surace, J. and Takagi, T. and van Kampen, E. (2008) The SCUBA Half-Degree Extragalactic Survey (SHADES) – VIII. the nature of faint submillimetre galaxies in SHADES, SWIRE and SXDF surveys. Monthly Notices of the Royal Astronomical Society, 387 (1). pp. 247-267. ISSN 0035-8711 http://resolver.caltech.edu/CaltechAUTHORS:20090424-093028091
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We present the optical-to-submillimetre spectral energy distributions (SEDs) for 33 radio and mid-infrared (mid-IR) identified submillimetre galaxies discovered via the SHADES 850-μm SCUBA imaging in the Subaru-XMM Deep Field (SXDF). Optical data for the sources come from the SXDF and mid- and far-IR fluxes from SWIRE. We obtain photometric redshift estimates for our sources using optical and IRAC 3.6- and 4.5-μm fluxes. We then fit SED templates to the longer wavelength data to determine the nature of the far-IR emission that dominates the bolometric luminosity of these sources. The IR template fits are also used to resolve ambiguous identifications and cases of redshift aliasing. The redshift distribution obtained broadly matches previous results for submillimetre sources and on the SHADES SXDF field. Our template fitting finds that active galactic nuclei, while present in about 10 per cent of our sources, do not contribute significantly to their bolometric luminosity. Dust heating by starbursts, with either Arp220 or M82 type SEDs, appears to be responsible for the luminosity in most sources (23/33 are fitted by Arp220 templates, 2/33 by the warmer M82 templates). 8/33 sources, in contrast, are fitted by a cooler cirrus dust template, suggesting that cold dust has a role in some of these highly luminous objects. Three of our sources appear to have multiple identifications or components at the same redshift, but we find no statistical evidence that close associations are common among our SHADES sources. Examination of rest-frame K-band luminosity suggests that ‘downsizing’ is underway in the submillimetre galaxy population, with lower redshift systems lying in lower mass host galaxies. Of our 33 identifications six are found to be of lower reliability but their exclusion would not significantly alter our conclusions.
|Additional Information:||©2008 The Authors. Journal compilation ©2008 RAS. Accepted 2008 March 2. Received 2008 February 7; in original form 2007 September 14. Thanks to Jeff Wagg and Marcos Trichas for useful comments. DLC is funded by PPARC/STFC, IS is supported by the Royal Society. The JCMT is supported by the United Kingdom Science and Technology Facilities Council (STFC), the National Research Council Canada (NRC), and the Netherlands Organization for Scientific Research(NWO); it is overseen by the JCMT Board.We acknowledge funding support from PPARC/STFC, NRC and NASA. The authors would like to thank the staff at the JCMT for their typically excellent support work. This research has made use of the NASA/IPAC Extragalactic Database (NED) which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration.|
|Subject Keywords:||galaxies: high-redshift; galaxies: infrared; galaxies: submillimetre|
|Usage Policy:||No commercial reproduction, distribution, display or performance rights in this work are provided.|
|Deposited By:||Joy Painter|
|Deposited On:||02 Jun 2009 23:58|
|Last Modified:||26 Dec 2012 10:58|
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