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

被引：96

作者：

Amblard, Alexandre ^{[1
]}

Cooray, Asantha ^{[1
]}

Serra, Paolo ^{[1
]}

Altieri, B. ^{[2
]}

Arumugam, V. ^{[3
]}

Aussel, H. ^{[4
]}

Blain, A.

Bock, J. ^{[5
]}

Boselli, A. ^{[6
]}

Buat, V. ^{[6
]}

Castro-Rodriguez, N. ^{[7
,8
]}

Cava, A. ^{[7
,8
]}

Chanial, P. ^{[9
]}

Chapin, E. ^{[10
]}

Clements, D. L. ^{[9
]}

Conley, A. ^{[11
]}

Conversi, L. ^{[2
]}

Dowell, C. D. ^{[5
]}

Dwek, E. ^{[12
]}

Eales, S. ^{[13
]}

Elbaz, D. ^{[4
]}

Farrah, D. ^{[14
]}

Franceschini, A. ^{[15
]}

Gear, W. ^{[13
]}

Glenn, J. ^{[11
]}

Griffin, M. ^{[13
]}

Halpern, M. ^{[10
]}

Hatziminaoglou, E. ^{[16
]}

Ibar, E. ^{[17
]}

Isaak, K. ^{[13
]}

Ivison, R. J. ^{[3
,17
]}

Khostovan, A. A. ^{[1
]}

Lagache, G. ^{[18
,19
]}

Levenson, L. ^{[5
]}

Lu, N. ^{[20
]}

Madden, S. ^{[4
]}

Maffei, B. ^{[21
]}

Mainetti, G. ^{[15
]}

Marchetti, L. ^{[15
]}

Marsden, G. ^{[10
]}

Mitchell-Wynne, K. ^{[1
]}

Nguyen, H. T. ^{[5
]}

O'Halloran, B. ^{[9
]}

Oliver, S. J. ^{[14
]}

Omont, A. ^{[22
]}

Page, M. J. ^{[23
]}

Panuzzo, P. ^{[4
]}

Papageorgiou, A. ^{[13
]}

Pearson, C. P. ^{[23
,25
]}

Perez-Fournon, I. ^{[7
,8
]}

机构：

[1] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA

[2] European Space Astron Ctr, Herschel Sci Ctr, Madrid 28691, Spain

[3] Univ Edinburgh, Inst Astron, Royal Observ, Edinburgh EH9 3HJ, Midlothian, Scotland

[4] Univ Paris Diderot, CNRS, Lab AIM Paris Saclay, CEA DSM Irfu,CE Saclay, F-91191 Gif Sur Yvette, France

[5] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA

[6] Univ Aix Marseille, CNRS, OAMP, Lab Astrophys Marseille, F-13388 Marseille 13, France

[7] Inst Astrofis Canarias, E-38200 San Cristobal la Laguna, Tenerife, Spain

[8] Univ La Laguna, Dept Astrofis, E-38205 Tenerife, Spain

[9] Univ London Imperial Coll Sci Technol & Med, Blackett Lab, Astrophys Grp, London SW7 2AZ, England

[10] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada

[11] Univ Colorado, Dept Astrophys & Planetary Sci, CASA UCB 389, Boulder, CO 80309 USA

[12] NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Greenbelt, MD 20771 USA

[13] Cardiff Univ, Cardiff Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales

[14] Univ Sussex, Dept Phys & Astron, Ctr Astron, Brighton BN1 9QH, E Sussex, England

[15] Univ Padua, Dipartimento Astron, I-35122 Padua, Italy

[16] ESO, D-85748 Garching, Germany

[17] Royal Observ, UK Astron Technol Ctr, Edinburgh EH9 3HJ, Midlothian, Scotland

[18] Univ Paris 11, Inst Astrophys Spatiale, F-91405 Orsay, France

[19] CNRS, UMR 8617, F-91405 Orsay, France

[20] CALTECH, Jet Prop Lab, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA

[21] Univ Manchester, Sch Phys & Astron, Manchester M13 9PL, Lancs, England

[22] Univ Paris 06, CNRS, UMR7095, Inst Astrophys Paris, F-75014 Paris, France

[23] Rutherford Appleton Lab, Space Sci & Technol Dept, Didcot OX11 0QX, Oxon, England

[24] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England

[25] Univ Lethbridge, Inst Space Imaging Sci, Lethbridge, AB T1K 3M4, Canada

[26] Univ Hertfordshire, Ctr Astrophys Res, Hatfield AL10 9AB, Herts, England

来源：

NATURE | 2011年 / 470卷 / 7335期

关键词：

HERSCHEL-SPIRE INSTRUMENT; STAR-FORMATION; NUMBER COUNTS; HERMES; REDSHIFT; SPITZER; ATLAS; BIAS;

D O I：

10.1038/nature09771

中图分类号：

O [数理科学和化学]; P [天文学、地球科学]; Q [生物科学]; N [自然科学总论];

学科分类号：

07 ; 0710 ; 09 ;

摘要：

The extragalactic background light at far-infrared wavelengths(1-3) comes from optically faint, dusty, star-forming galaxies in the Universe with star formation rates of a few hundred solar masses per year(4). These faint, submillimetre galaxies are challenging to study individually because of the relatively poor spatial resolution of far-infrared telescopes(5,6). Instead, their average properties can be studied using statistics such as the angular power spectrum of the background intensity variations(7-10). A previous attempt(11) at measuring this power spectrum resulted in the suggestion that the clustering amplitude is below the level computed with a simple ansatz based on a halo model(12). Here we report excess clustering over the linear prediction at arcminute angular scales in the power spectrum of brightness fluctuations at 250, 350 and 500 mu m. From this excess, we find that submillimetre galaxies are located in dark matter haloes with a minimum mass, M-min, such that log(10)[M-min/M-circle dot] = 11.5(-0.2)(+0.7) at 350 mu m, where M-circle dot is the solar mass. This minimum dark matter halo mass corresponds to the most efficient mass scale for star formation in the Universe(13), and is lower than that predicted by semi-analytical models for galaxy formation(14).

引用

页码：510 / 512

页数：3

共 30 条

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