HerMES: Halo occupation number and bias properties of dusty galaxies from angular clustering measurements

被引：65

作者：

Cooray, A. ^{[1
]}

Amblard, A. ^{[1
]}

Wang, L. ^{[25
]}

Arumugam, V. ^{[24
]}

Auld, R. ^{[23
]}

Aussel, H. ^{[26
]}

Babbedge, T. ^{[17
]}

Blain, A.

Bock, J. ^{[16
]}

Boselli, A. ^{[20
]}

Buat, V. ^{[20
]}

Burgarella, D. ^{[20
]}

Castro-Rodriguez, N. ^{[19
]}

Cava, A. ^{[19
]}

Chanial, P. ^{[17
]}

Clements, D. L. ^{[17
]}

Conley, A. ^{[18
]}

Conversi, L. ^{[21
]}

Dowell, C. D. ^{[16
]}

Dwek, E. ^{[22
]}

Eales, S. ^{[23
]}

Elbaz, D. ^{[26
]}

Farrah, D. ^{[25
]}

Fox, M. ^{[17
]}

Franceschini, A. ^{[3
]}

Gear, W. ^{[23
]}

Glenn, J. ^{[18
]}

Griffin, M. ^{[23
]}

Halpern, M. ^{[4
]}

Hatziminaoglou, E. ^{[5
]}

Ibar, E. ^{[6
]}

Isaak, K. ^{[23
]}

Ivison, R. J. ^{[6
,24
]}

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

Lagache, G. ^{[7
,8
]}

Levenson, L. ^{[16
]}

Lu, N. ^{[2
]}

Madden, S. ^{[26
]}

Maffei, B. ^{[9
]}

Mainetti, G. ^{[3
]}

Marchetti, L. ^{[3
]}

Marsden, G. ^{[4
]}

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

Mortier, A. M. J. ^{[17
]}

Nguyen, H. T. ^{[16
]}

O'Halloran, B. ^{[17
]}

Oliver, S. J. ^{[25
]}

Omont, A. ^{[10
]}

Page, M. J. ^{[11
]}

Panuzzo, P. ^{[26
]}

机构：

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

[2] CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA

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

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

[5] ESO, D-85748 Garching, Germany

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

[7] Univ Paris 11, IAS, F-91405 Orsay, France

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

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

[10] Univ Paris 06, CNRS, UMR 7095, Inst Astrophys Paris, F-75014 Paris, France

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

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

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

[14] Univ Oxford, Oxford OX1 3RH, England

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

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

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

[18] Univ Colorado, Dept Astrophys & Planetary Sci, Boulder, CO 80309 USA

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

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

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

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

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

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

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

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

来源：

ASTRONOMY & ASTROPHYSICS | 2010年 / 518卷

关键词：

submillimeter: galaxies; large-scale structure of Universe; cosmology: observations; galaxies: evolution; galaxies: high-redshift; STAR-FORMATION HISTORY; COUNTS; POPULATION; EVOLUTION;

D O I：

10.1051/0004-6361/201014597

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We measure the angular correlation function, omega(theta), from 0.5 to 30 arcmin of detected sources in two wide fields of the Herschel Multi-tiered Extragalactic Survey (HerMES). Our measurements are consistent with the expected clustering shape from a population of sources that trace the dark matter density field, including non-linear clustering at arcminute angular scales arising from multiple sources that occupy the same dark matter halos. By making use of the halo model to connect the spatial clustering of sources to the dark matter halo distribution, we estimate source bias and halo occupation number for dusty sub-mm galaxies at z similar to 2. We find that sub-mm galaxies with 250 mu m flux densities above 30 mJy reside in dark matter halos with mass above (5 +/- 4) x 10(12) M-circle dot, while (14 +/- 8)% of such sources appear as satellites in more massive halos.

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