The galaxy-halo connection from a joint lensing, clustering and abundance analysis in the CFHTLenS/VIPERS field

被引：125

作者：

Coupon, J. ^{[1
]}

Arnouts, S. ^{[2
]}

van Waerbeke, L. ^{[3
]}

Moutard, T. ^{[2
]}

Ilbert, O. ^{[2
]}

van Uitert, E. ^{[4
]}

Erben, T. ^{[4
]}

Garilli, B. ^{[5
]}

Guzzo, L. ^{[6
,7
]}

Heymans, C. ^{[8
]}

Hildebrandt, H. ^{[4
]}

Hoekstra, H. ^{[9
]}

Kilbinger, M. ^{[10
]}

Kitching, T. ^{[11
]}

Mellier, Y. ^{[10
,12
,13
]}

Miller, L. ^{[14
]}

Scodeggio, M. ^{[5
]}

Bonnett, C. ^{[15
]}

Branchini, E. ^{[16
,17
,18
]}

Davidzon, I. ^{[19
,20
]}

De Lucia, G. ^{[21
]}

Fritz, A. ^{[5
]}

Fu, L. ^{[22
]}

Hudelot, P. ^{[12
]}

Hudson, M. J. ^{[23
,24
]}

Kuijken, K. ^{[9
]}

Leauthaud, A. ^{[25
]}

Le Fevre, O. ^{[2
]}

McCracken, H. J. ^{[12
,13
]}

Moscardini, L. ^{[19
,20
,26
]}

Rowe, B. T. P. ^{[27
]}

Schrabback, T. ^{[4
]}

Semboloni, E. ^{[4
]}

Velander, M. ^{[14
]}

机构：

[1] Univ Geneva, Astron Observ, CH-1290 Versoix, Switzerland

[2] Aix Marseille Univ, CNRS, LAM, UMR 7326, F-13388 Marseille, France

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

[4] Univ Bonn, Argelander Inst Astron, D-53121 Bonn, Germany

[5] INAF Ist Astrofis Spaziale & Fis Cosm Milano, I-20133 Milan, Italy

[6] INAF Osservatorio Astron Brera, I-23807 Merate, Italy

[7] Univ Milano Bicocca, Dipartimento Fis 3, I-20126 Milan, Italy

[8] Univ Edinburgh, Inst Astron, Scottish Univ Phys Alliance, Edinburgh EH9 3HJ, Midlothian, Scotland

[9] Leiden Univ, Leiden Observ, NL-2333 CA Leiden, Netherlands

[10] CEA Saclay, Serv Astrophys SAp, F-91191 Gif Sur Yvette, France

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

[12] Univ Paris 06, UMR 7095, Inst Astrophys Paris, Sorbonne Univ, F-75014 Paris, France

[13] CNRS, UMR 7095, Inst Astrophys Paris, F-75014 Paris, France

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

[15] IFAE, E-08193 Bellaterra, Spain

[16] Univ Rome Tre, Dipartimento Matemat & Fis, I-00146 Rome, Italy

[17] Ist Nazl Fis Nucl, Sez Roma Tre, I-00146 Rome, Italy

[18] INAF Osservatorio Astron Roma, I-00040 Monte Porzio Catone, RM, Italy

[19] Univ Bologna, Dipartimento Fis & Astron, I-40127 Bologna, Italy

[20] INAF Osservatorio Astron Bologna, I-40127 Bologna, Italy

[21] INAF Osservatorio Astron Trieste, I-34143 Trieste, Italy

[22] Shanghai Normal Univ, Shanghai Key Lab Astrophys, Shanghai 200234, Peoples R China

[23] Univ Waterloo, Dept Phys & Astron, Waterloo, ON N2L 3G1, Canada

[24] Perimeter Inst Theoret Phys, Waterloo, ON N2L 1Y5, Canada

[25] Univ Tokyo, Todai Inst Adv Study, Kavli Inst Phys & Math Universe, Kashiwa, Chiba 2778583, Japan

[26] Ist Nazl Fis Nucl, Sez Bologna, I-40127 Bologna, Italy

[27] UCL, Dept Phys & Astron, London WC1E 6BT, England

来源：

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY | 2015年 / 449卷 / 02期

基金：

加拿大自然科学与工程研究理事会; 欧洲研究理事会;

关键词：

gravitational lensing: weak; galaxies: clusters: general; cosmology: observations; dark matter; REDSHIFT SURVEY VIPERS; STELLAR MASS FUNCTION; LARGE-SCALE STRUCTURE; DIGITAL SKY SURVEY; HUBBLE-DEEP-FIELD; DARK-MATTER HALOS; PHOTOMETRIC REDSHIFTS; OCCUPATION DISTRIBUTION; SHAPE MEASUREMENT; STAR-FORMATION;

D O I：

10.1093/mnras/stv276

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We present new constraints on the relationship between galaxies and their host dark matter haloes, measured from the location of the peak of the stellar-to-halo mass ratio (SHMR), up to the most massive galaxy clusters at redshift z similar to 0.8 and over a volume of nearly 0.1 Gpc(3). We use a unique combination of deep observations in the CFHTLenS/VIPERS field from the near-UV to the near-IR, supplemented by similar to 60 000 secure spectroscopic redshifts, analysing galaxy clustering, galaxy-galaxy lensing and the stellar mass function. We interpret our measurements within the halo occupation distribution (HOD) framework, separating the contributions from central and satellite galaxies. We find that the SHMRfor the central galaxies peaks at M-h,M- peak = 1.9(-0.1)(+0.2) x 10(12) M-circle dot with an amplitude of 0.025, which decreases to similar to 0.001 for massive haloes (M-h > 10(14) M-circle dot). Compared to central galaxies only, the total SHMR (including satellites) is boosted by a factor of 10 in the high-mass regime (cluster-size haloes), a result consistent with cluster analyses from the literature based on fully independent methods. After properly accounting for differences in modelling, we have compared our results with a large number of results from the literature up to z = 1: we find good general agreement, independently of the method used, within the typical stellar-mass systematic errors at low to intermediate mass (M-star < 10(11) M-circle dot) and the statistical errors above. We have also compared our SHMR results to semi-analytic simulations and found that the SHMR is tilted compared to our measurements in such a way that they over- (under-) predict star formation efficiency in central (satellite) galaxies.

引用

页码：1352 / 1379

页数：28

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