AzTEC millimetre survey of the COSMOS field – III. Source catalogue over 0.72 deg2 and plausible boosting by large-scale structure

  1. I. Aretxaga1,*,
  2. G. W. Wilson2,
  3. E. Aguilar1,
  4. S. Alberts2,
  5. K. S. Scott3,
  6. N. Scoville4,
  7. M. S. Yun2,
  8. J. Austermann5,
  9. T. P. Downes4,
  10. H. Ezawa6,
  11. B. Hatsukade7,
  12. D. H. Hughes1,
  13. R. Kawabe7,
  14. K. Kohno8,
  15. T. Oshima7,
  16. T. A. Perera9,
  17. Y. Tamura7,
  18. M. Zeballos1

Article first published online: 19 JUL 2011

DOI: 10.1111/j.1365-2966.2011.18989.x

Issue

Monthly Notices of the Royal Astronomical Society

Monthly Notices of the Royal Astronomical Society

Volume 415, Issue 4, pages 3831–3850, August 2011

Additional Information

How to Cite

Aretxaga, I., Wilson, G. W., Aguilar, E., Alberts, S., Scott, K. S., Scoville, N., Yun, M. S., Austermann, J., Downes, T. P., Ezawa, H., Hatsukade, B., Hughes, D. H., Kawabe, R., Kohno, K., Oshima, T., Perera, T. A., Tamura, Y. and Zeballos, M. (2011), AzTEC millimetre survey of the COSMOS field – III. Source catalogue over 0.72 deg2 and plausible boosting by large-scale structure. Monthly Notices of the Royal Astronomical Society, 415: 3831–3850. doi: 10.1111/j.1365-2966.2011.18989.x

Author Information

  1. 1

    Instituto Nacional de Astrofísica, Óptica y Electrónica (INAOE), Aptdo. Postal 51 y 216, 72000 Puebla, Pue., Mexico

  2. 2

    Department of Astronomy, University of Massachusetts, Amherst, MA 01003, USA

  3. 3

    Department of Physics and Astronomy, University of Pennsylvania, Philadelphia, PA 19104, USA

  4. 4

    California Institute of Technology, Pasadena, CA 91125, USA

  5. 5

    Center for Astrophysics and Space Astronomy, University of Colorado, Boulder, CO 80309, USA

  6. 6

    ALMA Project Office, National Astronomical Observatory of Japan, 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan

  7. 7

    Nobeyama Radio Observatory, Minamimaki, Minamisaku, Nagano 384-1305, Japan

  8. 8

    Institute of Astronomy, University of Tokyo, 2-21-1 Osawa, Mitaka, Tokyo 181-0015, Japan

  9. 9

    Department of Physics, Illinois Wesleyan University, Bloomington, IL 61701, USA

* E-mail: itziar@inaoep.mx

Publication History

  1. Issue published online: 18 AUG 2011
  2. Article first published online: 19 JUL 2011
  3. Accepted 2011 April 28. Received 2011 April 26; in original form 2011 February 4
Corrected by:

Erratum: AzTEC millimetre survey of the COSMOS field – III. Source catalogue over 0.72 deg2 and plausible boosting by large-scale structure

Vol. 419, Issue 2, 1824, Article first published online: 5 DEC 2011

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Keywords:

  • surveys;
  • galaxies: evolution;
  • cosmology: miscellaneous;
  • submillimetre: galaxies

ABSTRACT

We present a 0.72 deg2 contiguous 1.1-mm survey in the central area of the Cosmological Evolution Survey field carried out to a 1σ≈ 1.26 mJy beam−1 depth with the AzTEC camera mounted on the 10-m Atacama Submillimeter Telescope Experiment. We have uncovered 189 candidate sources at a signal-to-noise ratio (S/N) ≥ 3.5, out of which 129, with S/N ≥ 4, can be considered to have little chance of being spurious (≲2 per cent). We present the number counts derived with this survey, which show a significant excess of sources when compared to the number counts derived from the ∼0.5 deg2 area sampled at similar depths in the Submillimetre Common-User Bolometer Array (SCUBA) HAlf Degree Extragalactic Survey (SHADES). They are, however, consistent with those derived from fields that were considered too small to characterize the overall blank-field population. We identify differences to be more significant in the S1.1mm≳ 5 mJy regime, and demonstrate that these excesses in number counts are related to the areas where galaxies at redshifts z≲ 1.1 are more densely clustered. The positions of optical–infrared galaxies in the redshift interval 0.6 ≲z≲ 0.75 are the ones that show the strongest correlation with the positions of the 1.1-mm bright population (S1.1mm≳ 5 mJy), a result which does not depend exclusively on the presence of rich clusters within the survey sampled area. The most likely explanation for the observed excess in number counts at 1.1-mm is galaxy–galaxy and galaxy–group lensing at moderate amplification levels, which increases in amplitude as one samples larger and larger flux densities. This effect should also be detectable in other high-redshift populations.

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