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Published April 2015 | Published + Submitted
Journal Article Open

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


The relation between the galaxy stellar mass M⋆ 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 ~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⋆ and compute the SMHR = M⋆/M_h. We find that the SMHR ranges from 1% to 2.5% for galaxies with M⋆ = 1.3 × 10^9 M⊙ to M⋆ = 7.4 × 10^9 M⊙ in DM halos with M_h = 1.3 × 10^(11) M⊙ to M_h = 3 × 10^(11) M⊙. 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 ~ 7 × 10^9 M⊙. 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 ~ 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 ~ 3 begins to experience truncation of its star formation within a few million years.

Additional Information

© 2015 ESO. Article published by EDP Sciences. Received 17 December 2014; Accepted 27 February 2015; Published online 23 March 2015. We thank Jean Coupon and Carlo Schimd for interesting discussions. This work is supported by the European Research Council Advanced Grant ERC-2010-AdG-268107-EARLY, and by INAF Grants PRIN 2010&2012 and PICS 2013. A.C., O.C., M.T. and V.S. acknowledge the grant MIUR PRIN 2010–2011. This work is supported by the OCEVU Labex (ANR-11-LABX-0060) and the A*MIDEX project (ANR-11-IDEX-0001-02). A.P. is supported by grant UMO-2012/07/B/ST9/04425 and the Polish-Swiss Astro Project. Research conducted within the scope of the HECOLS International Associated Laboratory, supported in part by the Polish NCN grant Dec-2013/08/M/ST9/00664. This work is based on data products made available at the CESAM data center, Laboratoire d'Astrophysique de Marseille, France.

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Published - aa25532-14.pdf

Submitted - 1412.5584v1.pdf


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