Which haloes host Herschel-ATLAS galaxies in the local Universe?

被引：14

作者：

Guo, Qi ^{[19
]}

Cole, Shaun ^{[19
]}

Lacey, Cedric G. ^{[19
]}

Baugh, Carlton M. ^{[19
]}

Frenk, Carlos S. ^{[19
]}

Norberg, Peder ^{[1
]}

Auld, R. ^{[2
]}

Baldry, I. K. ^{[3
]}

Bamford, S. P. ^{[4
]}

Bourne, N. ^{[4
]}

Buttiglione, E. S. ^{[5
]}

Cava, A. ^{[6
,20
]}

Cooray, A. ^{[7
]}

Croom, S. ^{[8
]}

Dariush, A. ^{[2
]}

De Zotti, G. ^{[5
,9
]}

Driver, S. ^{[10
]}

Dunne, L. ^{[4
]}

Dye, S. ^{[2
]}

Eales, S. ^{[2
]}

Fritz, J. ^{[11
]}

Hopkins, A. ^{[12
]}

Hopwood, R. ^{[13
]}

Ibar, E. ^{[14
]}

Ivison, R. J. ^{[14
]}

Jarvis, M. ^{[15
]}

Jones, D. H. ^{[12
]}

Kelvin, L. ^{[10
]}

Liske, J. ^{[16
]}

Loveday, J. ^{[18
]}

Maddox, S. J. ^{[4
]}

Parkinson, H. ^{[1
]}

Pascale, E. ^{[2
]}

Peacock, J. A. ^{[1
]}

Pohlen, M. ^{[2
]}

Prescott, M. ^{[3
]}

Rigby, E. E. ^{[4
]}

Robotham, A. ^{[10
]}

Rodighiero, G. ^{[5
]}

Sharp, R. ^{[12
]}

Smith, D. J. B. ^{[2
]}

Temi, P. ^{[17
]}

van Kampen, E. ^{[16
]}

机构：

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

[2] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, Wales

[3] Liverpool John Moores Univ, Astrophys Res Inst, Birkenhead CH41 1LD, Merseyside, England

[4] Univ Nottingham, Sch Phys & Astron, Nottingham NG7 2RD, England

[5] Osserv Astron Padova, INAF, I-35122 Padua, Italy

[6] Inst Astrofis Canarias IAC, Tenerife, Spain

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

[8] Univ Sydney, Sydney Inst Astron, Sch Phys, Sydney, NSW 2006, Australia

[9] SISSA, I-34136 Trieste, Italy

[10] Univ St Andrews, Sch Phys & Astron, St Andrews KY16 9SS, Fife, Scotland

[11] Univ Ghent, Sterrenkundig Observatorium, B-9000 Ghent, Belgium

[12] Australian Astron Observ, Epping, NSW 1710, Australia

[13] Open Univ, Dept Phys & Astron, Milton Keynes MK7 6AA, Bucks, England

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

[15] Univ Hertfordshire, Sci & Technol Res Inst, Ctr Astrophys, Hatfield AL10 9AB, Herts, England

[16] European So Observ, D-85748 Garching, Germany

[17] NASA, Astrophys Branch, Ames Res Ctr, Moffett Field, CA 94035 USA

[18] Univ Sussex, Ctr Astron, Brighton BN1 9QH, E Sussex, England

[19] Univ Durham, Dept Phys, Inst Computat Cosmol, Durham DH1 3LE, England

[20] Dept Astrofis La Laguna ULL, Tenerife, Spain

来源：

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY | 2011年 / 412卷 / 04期

基金：

英国科学技术设施理事会;

关键词：

galaxies: haloes; dark matter; infrared: galaxies; STAR-FORMATION RATES; MASS ASSEMBLY GAMA; LUMINOSITY FUNCTION; NUMBER; SPIRE; BIAS;

D O I：

10.1111/j.1365-2966.2010.18051.x

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We measure the projected cross-correlation between low-redshift (z < 0.5) far-infrared selected galaxies in the science demonstration phase (SDP) field of the Herschel-ATLAS (H-ATLAS) survey and optically selected galaxies from the Galaxy and Mass Assembly (GAMA) redshift survey. In order to obtain robust correlation functions, we restrict the analysis to a subset of 969 out of 6900 H-ATLAS galaxies, which have reliable optical counterparts with r < 19.4 mag and well-determined spectroscopic redshifts. The overlap region between the two surveys is 12.6 deg2; the matched sample has a median redshift of z approximate to 0.2. The cross-correlation of GAMA and H-ATLAS galaxies within this region can be fitted by a power law, with correlation length r(0) approximate to 4.63 +/- 0.51 Mpc. Comparing with the corresponding autocorrelation function of GAMA galaxies within the SDP field yields a relative bias (averaged over 2-8 Mpc) of H-ATLAS and GAMA galaxies of b(H)/b(G) approximate to 0.6. Combined with clustering measurements from previous optical studies, this indicates that most of the low-redshift H-ATLAS sources are hosted by haloes with masses comparable to that of the Milky Way. The correlation function appears to depend on the 250-mu m luminosity, L-250, with bright (median luminosity nu L-250 similar to 1.6 x 1010 L-circle dot) objects being somewhat more strongly clustered than faint (nu L-250 similar to 4.0 x 109 L-circle dot) objects. This implies that galaxies with higher dust-obscured star formation rates are hosted by more massive haloes.

引用

页码：2277 / 2285

页数：9

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