dc.contributor.author | Geach, J. E. | en_US |
dc.contributor.author | Chapin, E. L. | en_US |
dc.contributor.author | Coppin, K. E. K. | en_US |
dc.contributor.author | Dunlop, J. S. | en_US |
dc.contributor.author | Halpern, M. | en_US |
dc.contributor.author | Smail, Ian | en_US |
dc.contributor.author | van der Werf, P. | en_US |
dc.contributor.author | Serjeant, S. | en_US |
dc.contributor.author | Farrah, D. | en_US |
dc.contributor.author | Roseboom, I. | en_US |
dc.contributor.author | Targett, T. | en_US |
dc.contributor.author | Arumugam, V. | en_US |
dc.contributor.author | Asboth, V. | en_US |
dc.contributor.author | Blain, A. | en_US |
dc.contributor.author | Chrysostomou, A. | en_US |
dc.contributor.author | Clarke, C. | en_US |
dc.contributor.author | Ivison, R. J. | en_US |
dc.contributor.author | Jones, S. L. | en_US |
dc.contributor.author | Karim, A. | en_US |
dc.contributor.author | Mackenzie, T. | en_US |
dc.contributor.author | Meijerink, R. | en_US |
dc.contributor.author | Michalowski, M. J. | en_US |
dc.contributor.author | Scott, D. | en_US |
dc.contributor.author | Simpson, J. | en_US |
dc.contributor.author | Swinbank, A. M. | en_US |
dc.contributor.author | Alexander, D. | en_US |
dc.contributor.author | Almaini, O. | en_US |
dc.contributor.author | Aretxaga, I. | en_US |
dc.contributor.author | Best, P. | en_US |
dc.contributor.author | Chapman, S. | en_US |
dc.contributor.author | Clements, D. L. | en_US |
dc.contributor.author | Conselice, C. | en_US |
dc.contributor.author | Danielson, A. L. R. | en_US |
dc.contributor.author | Eales, S. | en_US |
dc.contributor.author | Edge, A. C. | en_US |
dc.contributor.author | Gibb, A. | en_US |
dc.contributor.author | Hughes, D. | en_US |
dc.contributor.author | Jenness, T. | en_US |
dc.contributor.author | Knudsen, K. K. | en_US |
dc.contributor.author | Lacey, C. | en_US |
dc.contributor.author | Marsden, G. | en_US |
dc.contributor.author | McMahon, R. | en_US |
dc.contributor.author | Oliver, S. | en_US |
dc.contributor.author | Page, M. J. | en_US |
dc.contributor.author | Peacock, J. A. | en_US |
dc.contributor.author | Rigopoulou, D. | en_US |
dc.contributor.author | Robson, E. I. | en_US |
dc.contributor.author | Spaans, M. | en_US |
dc.contributor.author | Stevens, J. | en_US |
dc.contributor.author | Webb, T. M. A. | en_US |
dc.contributor.author | Willott, C. | en_US |
dc.contributor.author | Wilson, C. D. | en_US |
dc.contributor.author | Zemcov, M. | en_US |
dc.date.accessioned | 2014-03-12T19:20:51Z | |
dc.date.available | 2014-03-12T19:20:51Z | |
dc.date.issued | 2012-11-28 | en_US |
dc.identifier.citation | Geach, J. E., E. L. Chapin, K. E. K. Coppin, J. S. Dunlop, et al. 2012. "The SCUBA-2 Cosmology Legacy Survey: blank-field number counts of 450um-selected galaxies and their contribution to the cosmic infrared background." Monthly Notices of the Royal Astronomical Society 432:53. | en_US |
dc.identifier.issn | 0035-8711 | |
dc.identifier.uri | http://hdl.handle.net/10222/45307 | |
dc.identifier.uri | http://dx.doi.org/10.1093/mnras/stt352 | |
dc.description.abstract | The first deep blank-field 450um map (1-sigma~1.3mJy) from the SCUBA-2 Cosmology Legacy Survey (S2CLS), conducted with the James Clerk Maxwell Telescope (JCMT) is presented. Our map covers 140 arcmin^2 of the COSMOS field, in the footprint of the HST CANDELS area. Using 60 submillimetre galaxies (SMGs) detected at >3.75-sigma, we evaluate the number counts of 450um-selected galaxies with flux densities S_450>5mJy. The 8-arcsec JCMT beam and high sensitivity of SCUBA-2 now make it possible to directly resolve a larger fraction of the cosmic infrared background (CIB, peaking at ~200um) into the individual galaxies responsible for its emission than has previously been possible at this wavelength. At S_450>5mJy we resolve (7.4[+/-]0.7)x10^-2 MJy/sr of the CIB at 450um (equivalent to 16[+/-]7% of the absolute brightness measured by COBE at this wavelength) into point sources. A further ~40% of the CIB can be recovered through a statistical stack of 24um emitters in this field, indicating that the majority (~60%) of the CIB at 450um is emitted by galaxies with S_450>2mJy. The average redshift of 450um emitters identified with an optical/near-infrared counterpart is estimated to be =1.3, implying that the galaxies in the sample are in the ultraluminous class (L_IR~1.1x10^12 L_sun). If the galaxies contributing to the statistical stack lie at similar redshifts, then the majority of the CIB at 450um is emitted by galaxies in the LIRG class with L_IR>3.6x10^11 L_sun. | en_US |
dc.relation.ispartof | Monthly Notices of the Royal Astronomical Society | |
dc.title | The SCUBA-2 Cosmology Legacy Survey: blank-field number counts of 450um-selected galaxies and their contribution to the cosmic infrared background | en_US |
dc.title.alternative | arXiv:1211.6668 [astro-ph] | en_US |
dc.type | article | en_US |
dc.identifier.volume | 432 | |
dc.identifier.startpage | 53 | en_US |