Stellar mass to halo mass relation from galaxy clustering in VUDS: a high star formation efficiency at z ≃ 3

被引：21

作者：

Durkalec, A. ^{[1
]}

Le Fevre, O. ^{[1
]}

de la Torre, S. ^{[1
]}

Pollo, A. ^{[19
,20
]}

Cassata, P. ^{[1
,18
]}

Garilli, B. ^{[3
]}

Le Brun, V. ^{[1
]}

Lemaux, B. C. ^{[1
]}

Maccagni, D. ^{[3
]}

Pentericci, L. ^{[4
]}

Tasca, L. A. M. ^{[1
]}

Thomas, R. ^{[1
]}

Vanzella, E. ^{[2
]}

Zamorani, G. ^{[2
]}

Zucca, E. ^{[2
]}

Amorin, R. ^{[4
]}

Bardelli, S. ^{[2
]}

Cassara, L. P. ^{[3
]}

Castellano, M. ^{[4
]}

Cimatti, A. ^{[5
]}

Cucciati, O. ^{[2
,5
]}

Fontana, A. ^{[4
]}

Giavalisco, M. ^{[13
]}

Grazian, A. ^{[4
]}

Hathi, N. P. ^{[1
]}

Ilbert, O. ^{[1
]}

Paltani, S. ^{[9
]}

Ribeiro, B. ^{[1
]}

Schaerer, D. ^{[8
,10
]}

Scodeggio, M. ^{[3
]}

Sommariva, V. ^{[4
,5
]}

Talia, M. ^{[5
]}

Tresse, L. ^{[1
]}

Vereani, D. ^{[2
,6
]}

Capak, P. ^{[12
]}

Charlot, S. ^{[7
]}

Contini, T. ^{[8
]}

Cuby, J. G. ^{[1
]}

Dunlop, J. ^{[16
]}

Fotopoulou, S. ^{[9
]}

Koekemoer, A. ^{[17
]}

Lopez-Sanjuan, C. ^{[11
]}

Mellier, Y. ^{[7
]}

Pforr, J. ^{[1
]}

Salvato, M. ^{[14
]}

Scoville, N. ^{[12
]}

Taniguchi, Y. ^{[15
]}

Wang, P. W. ^{[1
]}

机构：

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

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

[3] INAF IASF, I-20133 Milan, Italy

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

[5] Univ Bologna, Dept Phys & Astron DIFA, I-40127 Bologna, Italy

[6] INAF IASF Bologna, I-40129 Bologna, Italy

[7] Univ Paris 06, CNRS, UMR7095, Inst Astrophys Phys, Paris, France

[8] Univ Toulouse, UPS OMP, CNRS, IRAP, F-31400 Toulouse, France

[9] Univ Geneva, Dept Astron, CH-1290 Versoix, Switzerland

[10] Univ Geneva, Observ Geneva, CH-1290 Versoix, Switzerland

[11] Ctr Estudios Fis Cosmos Aragon, Teruel 44001, Spain

[12] CALTECH, Dept Astron, Pasadena, CA 91125 USA

[13] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA

[14] Max Planck Inst Extraterr Phys, D-85741 Garching, Germany

[15] Ehime Univ, Res Ctr Space & Cosm Evolut, Matsuyama, Ehime 7908577, Japan

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

[17] Space Telescope Sci Inst, Baltimore, MD 21218 USA

[18] Univ Valparaiso, Fac Ciencias, Inst Fis & Astron, Valparaiso, Chile

[19] Jagiellonian Univ, Astron Observ, PL-30001 Krakow, Poland

[20] Natl Ctr Nucl Res, PL-00681 Warsaw, Poland

来源：

ASTRONOMY & ASTROPHYSICS | 2015年 / 576卷

基金：

欧洲研究理事会;

关键词：

large-scale structure of Universe; early Universe; galaxies: evolution; methods: statistical; DARK-MATTER; EVOLUTION; UNCERTAINTIES; ENVIRONMENT; LUMINOSITY; HISTORIES; RATES;

D O I：

10.1051/0004-6361/201425532

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

The relation between the galaxy stellar mass M-star and the dark matter halo mass M-h gives important information on the efficiency in forming stars and assembling stellar mass in galaxies. We present measurements of the ratio of stellar mass to halo mass (SMHR) at redshifts 2 < z < 5, obtained from the VIMOS Ultra Deep Survey. We use halo occupation distribution (HOD) modelling of clustering measurements on similar to 3000 galaxies with spectroscopic redshifts to derive the dark matter halo mass M-h, and spectral energy density fitting over a large set of multi-wavelength data to derive the stellar mass M-star and compute the SMHR = M-star/M-h. We find that the SMHR ranges from 1% to 2.5% for galaxies with M-star = 1.3 x 10(9) M-star to M-star = 7.4 x 10(9) M-circle dot in DM halos with M-h = 1.3 x 10(11) M-circle dot to M-h = 3 x 10(11) M-circle dot. We derive the integrated star formation efficiency (ISFE) of these galaxies and find that the star formation efficiency is a moderate 6-9% for lower mass galaxies, while it is relatively high at 16% for galaxies with the median stellar mass of the sample similar to 7 x 10(9) M-circle dot. The lower ISFE at lower masses may indicate that some efficient means of suppressing star formation is at work (like SNe feedback), while the high ISFE for the average galaxy at z similar to 3 indicates that these galaxies efficiently build up their stellar mass at a key epoch in the mass assembly process. Based on our results, we propose a possible scenario in which the average massive galaxy at z similar to 3 begins to experience truncation of its star formation within a few million years.

引用

页数：4

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