University of Hertfordshire

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  • J. A. Zavala
  • I. Aretxaga
  • J. E. Geach
  • M. Birkinshaw
  • E. Chapin
  • S. Chapman
  • Chian-Chou Chen
  • D. L. Clements
  • J. S. Dunlop
  • D. Farrah
  • R. J. Ivison
  • T. Jenness
  • M. J. Michałowski
  • E. I. Robson
  • Douglas Scott
  • J. Simpson
  • M. Spaans
  • P. van der Werf
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Original languageEnglish
Pages (from-to)3369-3384
Number of pages16
JournalMonthly Notices of the Royal Astronomical Society
Volume464
Issue3
Early online date13 Oct 2016
DOIs
Publication statusPublished - 21 Jan 2017

Abstract

We present deep observations at 450 um and 850 um in the Extended Groth Strip field taken with the SCUBA-2 camera mounted on the James Clerk Maxwell Telescope as part of the deep SCUBA-2 Cosmology Legacy Survey (S2CLS), achieving a central instrumental depth of $\sigma_{450}=1.2$ mJy/beam and $\sigma_{850}=0.2$ mJy/beam. We detect 57 sources at 450 um and 90 at 850 um with S/N > 3.5 over ~70 sq. arcmin. From these detections we derive the number counts at flux densities $S_{450}>4.0$ mJy and $S_{850}>0.9$ mJy, which represent the deepest number counts at these wavelengths derived using directly extracted sources from only blank-field observations with a single-dish telescope. Our measurements smoothly connect the gap between previous shallower blank-field single-dish observations and deep interferometric ALMA results. We estimate the contribution of our SCUBA-2 detected galaxies to the cosmic infrared background (CIB), as well as the contribution of 24 um-selected galaxies through a stacking technique, which add a total of $0.26\pm0.03$ and $0.07\pm0.01$ MJy/sr, at 450 um and 850 um, respectively. These surface brightnesses correspond to $60\pm20$ and $50\pm20$ per cent of the total CIB measurements, where the errors are dominated by those of the total CIB. Using the photometric redshifts of the 24 um-selected sample and the redshift distributions of the submillimetre galaxies, we find that the redshift distribution of the recovered CIB is different at each wavelength, with a peak at $z\sim1$ for 450 um and at $z\sim2$ for 850um, consistent with previous observations and theoretical models.

Notes

This article has been accepted for publication in Monthly Notices of the Royal Astronomical Society. ©: 2016 The Author (s). Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved.

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