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Herschel-ATLAS/GAMA: spatial clustering of low-redshift submm galaxies†

  1. E. van Kampen1,*,
  2. D. J. B. Smith2,3,
  3. S. Maddox2,4,
  4. A. M. Hopkins5,
  5. I. Valtchanov6,
  6. J. A. Peacock7,
  7. M. J. Michałowski7,
  8. P. Norberg8,
  9. S. Eales9,
  10. L. Dunne2,4,
  11. J. Liske1,
  12. M. Baes10,
  13. D. Scott11,
  14. E. Rigby2,7,
  15. A. Robotham12,
  16. P. van der Werf7,13,
  17. E. Ibar14,
  18. M. J. Jarvis3,
  19. J. Loveday15,
  20. R. Auld7,
  21. I. K. Baldry16,
  22. S. Bamford2,
  23. E. Cameron17,
  24. S. Croom18,
  25. S. Buttiglione19,
  26. A. Cava20,
  27. A. Cooray21,
  28. S. Driver12,22,
  29. J. S. Dunlop7,
  30. A. Dariush23,
  31. J. Fritz10,
  32. R. J. Ivison14,
  33. E. Pascale9,
  34. M. Pohlen9,
  35. G. Rodighiero24,
  36. P. Temi25,
  37. D. G. Bonfield3,
  38. D. Hill3,
  39. D. H. Jones5,
  40. L. Kelvin12,
  41. H. Parkinson7,
  42. M. Prescott16,
  43. R. Sharp5,
  44. G. de Zotti19,26,
  45. S. Serjeant27,
  46. C. C. Popescu28,
  47. R. J. Tuffs29

Article first published online: 22 OCT 2012

DOI: 10.1111/j.1365-2966.2012.21949.x

Issue

Monthly Notices of the Royal Astronomical Society

Monthly Notices of the Royal Astronomical Society

Volume 426, Issue 4, pages 3455–3463, 11 November 2012

Additional Information

How to Cite

van Kampen, E., Smith, D. J. B., Maddox, S., Hopkins, A. M., Valtchanov, I., Peacock, J. A., Michałowski, M. J., Norberg, P., Eales, S., Dunne, L., Liske, J., Baes, M., Scott, D., Rigby, E., Robotham, A., van der Werf, P., Ibar, E., Jarvis, M. J., Loveday, J., Auld, R., Baldry, I. K., Bamford, S., Cameron, E., Croom, S., Buttiglione, S., Cava, A., Cooray, A., Driver, S., Dunlop, J. S., Dariush, A., Fritz, J., Ivison, R. J., Pascale, E., Pohlen, M., Rodighiero, G., Temi, P., Bonfield, D. G., Hill, D., Jones, D. H., Kelvin, L., Parkinson, H., Prescott, M., Sharp, R., de Zotti, G., Serjeant, S., Popescu, C. C. and Tuffs, R. J. (2012), Herschel-ATLAS/GAMA: spatial clustering of low-redshift submm galaxies. Monthly Notices of the Royal Astronomical Society, 426: 3455–3463. doi: 10.1111/j.1365-2966.2012.21949.x

Author Information

  1. 1

    European Southern Observatory, Garching bei München, Germany

  2. 2

    School of Physics and Astronomy, University of Nottingham, Nottingham

  3. 3

    Centre for Astrophysics Research, Science and Technology Research Institute, University of Hertfordshire, Herts

  4. 4

    Department of Physics and Astronomy, University of Canterbury, Christchurch, New Zealand

  5. 5

    Australian Astronomical Observatory, Epping, NSW 1710, Australia

  6. 6

    Herschel Science Centre, ESAC, ESA, Villanueva de la Cañada, 28691 Madrid, Spain

  7. 7

    SUPA, Institute for Astronomy, University of Edinburgh, Royal Observatory, Edinburgh

  8. 8

    Institute for Computational Cosmology, Department of Physics, Durham University, Durham

  9. 9

    School of Physics and Astronomy, Cardiff University, Cardiff

  10. 10

    Sterrenkundig Observatorium, Universiteit Gent, Gent, Belgium

  11. 11

    Department of Physics and Astronomy, 6224 Agricultural Road, University of British Columbia, Vancouver, BC, Canada

  12. 12

    SUPA, School of Physics and Astronomy, University of St. Andrews, North Haugh, St. Andrews

  13. 13

    Leiden Observatory, Leiden University, NL-2300 RA Leiden, the Netherlands

  14. 14

    UK Astronomy Technology Center, Royal Observatory Edinburgh, Edinburgh

  15. 15

    Astronomy Centre, Department of Physics and Astronomy, University of Sussex, Falmer, Brighton

  16. 16

    Astrophysics Research Institute, Liverpool John Moores University, Egerton Wharf, Birkenhead

  17. 17

    ETH Zurich, Insitute for Astronomy, Zurich, Switzerland

  18. 18

    Sydney Institute for Astronomy, School of Physics, University of Sydney, NSW, Australia

  19. 19

    INAF-Osservatorio Astronomico di Padova, Padova, Italy

  20. 20

    Departamento de Astrofísica, Facultad de CC. Físicas, Universidad Complutense de Madrid, Madrid, Spain

  21. 21

    Department of Physics & Astronomy, University of California, Irvine, CA, USA

  22. 22

    International Centre for Radio Astronomy Research (ICRAR), University of Western Australia, WA, Australia

  23. 23

    Physics Department, Imperial College London, London

  24. 24

    University of Padova, Padova, Italy

  25. 25

    Astrophysics Branch, NASA Ames Research Center, Moffett Field, CA, USA

  26. 26

    SISSA, Trieste, Italy

  27. 27

    Department of Physics and Astronomy, The Open University, Milton Keynes

  28. 28

    Jeremiah Horrocks Institute, University of Central Lancashire, Preston

  29. 29

    Max Planck Institute for Nuclear Astrophysics (MPIK), Heidelberg, Germany

*E-mail: evkampen@eso.org

  1. †

    Herschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA.

Publication History

  1. Issue published online: 17 OCT 2012
  2. Article first published online: 22 OCT 2012
  3. Manuscript Accepted: 15 AUG 2012
  4. Manuscript Received: 19 JUL 2012

Funded by

  • STFC (UK)
  • ARC (Australia)
  • AAO
  • Austrian Science Foundation FWF. Grant Numbers: P18493, I164

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Keywords:

  • surveys;
  • galaxies: statistics;
  • large-scale structure of Universe;
  • submillimetre: galaxies

ABSTRACT

We have measured the clustering properties of low-redshift (z < 0.3) submm galaxies detected at 250 μm in the Herschel-ATLAS science demonstration phase field. We selected a sample for which we have high-quality spectroscopic redshifts, obtained from reliably matching the 250-μm sources to a complete (for r < 19.4) sample of galaxies from the GAMA data base. Both the angular and spatial clustering strength are measured for all z < 0.3 sources as well as for five redshift slices with thickness Δz = 0.05 in the range 0.05 < z < 0.3. Our measured spatial clustering length r0 is comparable to that of optically selected, moderately star-forming (blue) galaxies: we find values around 5 Mpc. One of the redshift bins contains an interesting structure, at z = 0.164.

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