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Submillimetre galaxies reside in dark matter haloes with masses greater than 3 × 1011 solar masses

Author

Listed:
  • Alexandre Amblard

    (University of California)

  • Asantha Cooray

    (University of California
    California Institute of Technology, 1200 East California Boulevard)

  • Paolo Serra

    (University of California)

  • B. Altieri

    (Herschel Science Centre, European Space Astronomy Centre, Villanueva de la Cañada, 28691 Madrid, Spain)

  • V. Arumugam

    (Institute for Astronomy, University of Edinburgh, Royal Observatory, Blackford Hill, Edinburgh EH9 3HJ, UK)

  • H. Aussel

    (Laboratoire AIM-Paris-Saclay, CEA/DSM/Irfu - CNRS - Université Paris Diderot, CE-Saclay, pt courrier 131, F-91191 Gif-sur-Yvette, France)

  • A. Blain

    (California Institute of Technology, 1200 East California Boulevard)

  • J. Bock

    (California Institute of Technology, 1200 East California Boulevard
    Jet Propulsion Laboratory, 4800 Oak Grove Drive)

  • A. Boselli

    (Laboratoire d’Astrophysique de Marseille, OAMP, Université Aix-Marseille, CNRS, 38 rue Frédéric Joliot-Curie, 13388 Marseille cedex 13, France)

  • V. Buat

    (Laboratoire d’Astrophysique de Marseille, OAMP, Université Aix-Marseille, CNRS, 38 rue Frédéric Joliot-Curie, 13388 Marseille cedex 13, France)

  • N. Castro-Rodríguez

    (Instituto de Astrofísica de Canarias, E-38200 La Laguna, Tenerife, Spain
    Universidad de La Laguna, E-38205 La Laguna, Tenerife, Spain)

  • A. Cava

    (Instituto de Astrofísica de Canarias, E-38200 La Laguna, Tenerife, Spain
    Universidad de La Laguna, E-38205 La Laguna, Tenerife, Spain)

  • P. Chanial

    (Astrophysics Group, Imperial College London, Blackett Laboratory, Prince Consort Road, London SW7 2AZ, UK)

  • E. Chapin

    (University of British Columbia, 6224 Agricultural Road, Vancouver, British Columbia V6T 1Z1, Canada)

  • D. L. Clements

    (Astrophysics Group, Imperial College London, Blackett Laboratory, Prince Consort Road, London SW7 2AZ, UK)

  • A. Conley

    (CASA 389-UCB, University of Colorado)

  • L. Conversi

    (Herschel Science Centre, European Space Astronomy Centre, Villanueva de la Cañada, 28691 Madrid, Spain)

  • C. D. Dowell

    (California Institute of Technology, 1200 East California Boulevard
    Jet Propulsion Laboratory, 4800 Oak Grove Drive)

  • E. Dwek

    (Observational Cosmology Lab, Code 665, NASA Goddard Space Flight Center)

  • S. Eales

    (Cardiff School of Physics and Astronomy, Cardiff University, Queens Buildings, The Parade, Cardiff CF24 3AA, UK)

  • D. Elbaz

    (Laboratoire AIM-Paris-Saclay, CEA/DSM/Irfu - CNRS - Université Paris Diderot, CE-Saclay, pt courrier 131, F-91191 Gif-sur-Yvette, France)

  • D. Farrah

    (Astronomy Centre, University of Sussex, Brighton BN1 9QH, UK)

  • A. Franceschini

    (Università di Padova, Vicolo Osservatorio, 3, 35122 Padova, Italy)

  • W. Gear

    (Cardiff School of Physics and Astronomy, Cardiff University, Queens Buildings, The Parade, Cardiff CF24 3AA, UK)

  • J. Glenn

    (CASA 389-UCB, University of Colorado)

  • M. Griffin

    (Cardiff School of Physics and Astronomy, Cardiff University, Queens Buildings, The Parade, Cardiff CF24 3AA, UK)

  • M. Halpern

    (University of British Columbia, 6224 Agricultural Road, Vancouver, British Columbia V6T 1Z1, Canada)

  • E. Hatziminaoglou

    (ESO, Karl-Schwarzschild-Strasse 2, 85748 Garching bei München, Germany)

  • E. Ibar

    (UK Astronomy Technology Centre, Royal Observatory, Blackford Hill, Edinburgh EH9 3HJ, UK)

  • K. Isaak

    (Cardiff School of Physics and Astronomy, Cardiff University, Queens Buildings, The Parade, Cardiff CF24 3AA, UK)

  • R. J. Ivison

    (Institute for Astronomy, University of Edinburgh, Royal Observatory, Blackford Hill, Edinburgh EH9 3HJ, UK
    UK Astronomy Technology Centre, Royal Observatory, Blackford Hill, Edinburgh EH9 3HJ, UK)

  • A. A. Khostovan

    (University of California)

  • G. Lagache

    (Institut d’Astrophysique Spatiale, Bâtiment 121, Université Paris-Sud 11 and CNRS (UMR 8617), 91405 Orsay, France)

  • L. Levenson

    (California Institute of Technology, 1200 East California Boulevard
    Jet Propulsion Laboratory, 4800 Oak Grove Drive)

  • N. Lu

    (California Institute of Technology, 1200 East California Boulevard
    Infrared Processing and Analysis Center, MS 100-22, California Institute of Technology, JPL, Pasadena, California 91125, USA)

  • S. Madden

    (Laboratoire AIM-Paris-Saclay, CEA/DSM/Irfu - CNRS - Université Paris Diderot, CE-Saclay, pt courrier 131, F-91191 Gif-sur-Yvette, France)

  • B. Maffei

    (School of Physics and Astronomy, The University of Manchester, Alan Turing Building, Oxford Road, Manchester M13 9PL, UK)

  • G. Mainetti

    (Università di Padova, Vicolo Osservatorio, 3, 35122 Padova, Italy)

  • L. Marchetti

    (Università di Padova, Vicolo Osservatorio, 3, 35122 Padova, Italy)

  • G. Marsden

    (University of British Columbia, 6224 Agricultural Road, Vancouver, British Columbia V6T 1Z1, Canada)

  • K. Mitchell-Wynne

    (University of California)

  • H. T. Nguyen

    (California Institute of Technology, 1200 East California Boulevard
    Jet Propulsion Laboratory, 4800 Oak Grove Drive)

  • B. O’Halloran

    (Astrophysics Group, Imperial College London, Blackett Laboratory, Prince Consort Road, London SW7 2AZ, UK)

  • S. J. Oliver

    (Astronomy Centre, University of Sussex, Brighton BN1 9QH, UK)

  • A. Omont

    (Institut d’Astrophysique de Paris, UMR 7095, CNRS, UPMC Univ. Paris 06, 98bis Boulevard Arago, F-75014 Paris, France)

  • M. J. Page

    (Rutherford Appleton Laboratory, Chilton, Didcot OX11 0QX, UK)

  • P. Panuzzo

    (Laboratoire AIM-Paris-Saclay, CEA/DSM/Irfu - CNRS - Université Paris Diderot, CE-Saclay, pt courrier 131, F-91191 Gif-sur-Yvette, France)

  • A. Papageorgiou

    (Cardiff School of Physics and Astronomy, Cardiff University, Queens Buildings, The Parade, Cardiff CF24 3AA, UK)

  • C. P. Pearson

    (Rutherford Appleton Laboratory, Chilton, Didcot OX11 0QX, UK
    Institute for Space Imaging Science, University of Lethbridge, Lethbridge, Alberta T1K 3M4, Canada)

  • I. Pérez-Fournon

    (Instituto de Astrofísica de Canarias, E-38200 La Laguna, Tenerife, Spain
    Universidad de La Laguna, E-38205 La Laguna, Tenerife, Spain)

  • M. Pohlen

    (Cardiff School of Physics and Astronomy, Cardiff University, Queens Buildings, The Parade, Cardiff CF24 3AA, UK)

  • N. Rangwala

    (CASA 389-UCB, University of Colorado)

  • I. G. Roseboom

    (Astronomy Centre, University of Sussex, Brighton BN1 9QH, UK)

  • M. Rowan-Robinson

    (Astrophysics Group, Imperial College London, Blackett Laboratory, Prince Consort Road, London SW7 2AZ, UK)

  • M. Sánchez Portal

    (Herschel Science Centre, European Space Astronomy Centre, Villanueva de la Cañada, 28691 Madrid, Spain)

  • B. Schulz

    (California Institute of Technology, 1200 East California Boulevard
    Infrared Processing and Analysis Center, MS 100-22, California Institute of Technology, JPL, Pasadena, California 91125, USA)

  • Douglas Scott

    (University of British Columbia, 6224 Agricultural Road, Vancouver, British Columbia V6T 1Z1, Canada)

  • N. Seymour

    (Rutherford Appleton Laboratory, Chilton, Didcot OX11 0QX, UK)

  • D. L. Shupe

    (California Institute of Technology, 1200 East California Boulevard
    Infrared Processing and Analysis Center, MS 100-22, California Institute of Technology, JPL, Pasadena, California 91125, USA)

  • A. J. Smith

    (Astronomy Centre, University of Sussex, Brighton BN1 9QH, UK)

  • J. A. Stevens

    (Centre for Astrophysics Research, University of Hertfordshire, College Lane)

  • M. Symeonidis

    (Rutherford Appleton Laboratory, Chilton, Didcot OX11 0QX, UK)

  • M. Trichas

    (Astrophysics Group, Imperial College London, Blackett Laboratory, Prince Consort Road, London SW7 2AZ, UK)

  • K. Tugwell

    (Mullard Space Science Laboratory, University College London, Holmbury St Mary, Dorking RH5 6NT, UK)

  • M. Vaccari

    (Università di Padova, Vicolo Osservatorio, 3, 35122 Padova, Italy)

  • E. Valiante

    (University of British Columbia, 6224 Agricultural Road, Vancouver, British Columbia V6T 1Z1, Canada)

  • I. Valtchanov

    (Herschel Science Centre, European Space Astronomy Centre, Villanueva de la Cañada, 28691 Madrid, Spain)

  • J. D. Vieira

    (California Institute of Technology, 1200 East California Boulevard)

  • L. Vigroux

    (Institut d’Astrophysique de Paris, UMR 7095, CNRS, UPMC Univ. Paris 06, 98bis Boulevard Arago, F-75014 Paris, France)

  • L. Wang

    (Astronomy Centre, University of Sussex, Brighton BN1 9QH, UK)

  • R. Ward

    (Astronomy Centre, University of Sussex, Brighton BN1 9QH, UK)

  • G. Wright

    (UK Astronomy Technology Centre, Royal Observatory, Blackford Hill, Edinburgh EH9 3HJ, UK)

  • C. K. Xu

    (California Institute of Technology, 1200 East California Boulevard
    Infrared Processing and Analysis Center, MS 100-22, California Institute of Technology, JPL, Pasadena, California 91125, USA)

  • M. Zemcov

    (California Institute of Technology, 1200 East California Boulevard
    Jet Propulsion Laboratory, 4800 Oak Grove Drive)

Abstract

Galaxies in the background The optically faint 'submillimetre' star-forming galaxies that produce the extragalactic background light at far-infrared wavelengths are challenging to study individually, but their average properties can be determined using statistics such as the angular power spectrum of the background intensity variations. Using this technique, Amblard et al. have observed excess clustering over the linear prediction at arcminute angular scales in the power spectrum of brightness fluctuations at 250, 350 and 500 micrometres. This suggests that submillimetre galaxies are located in dark matter haloes with masses greater than 300 billion times that of the Sun, a direct measurement that will add useful detail to improve theoretical models of galaxy formation and evolution.

Suggested Citation

  • Alexandre Amblard & Asantha Cooray & Paolo Serra & B. Altieri & V. Arumugam & H. Aussel & A. Blain & J. Bock & A. Boselli & V. Buat & N. Castro-Rodríguez & A. Cava & P. Chanial & E. Chapin & D. L. Cle, 2011. "Submillimetre galaxies reside in dark matter haloes with masses greater than 3 × 1011 solar masses," Nature, Nature, vol. 470(7335), pages 510-512, February.
    • Handle: RePEc:nat:nature:v:470:y:2011:i:7335:d:10.1038_nature09771
    DOI: 10.1038/nature09771
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