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Published May 2013 | Published
Journal Article Open

Connecting stellar mass and star-formation rate to dark matter halo mass out to z ∼ 2


We have constructed an extended halo model (EHM) which relates the total stellar mass and star-formation rate (SFR) to halo mass (M_h). An empirical relation between the distribution functions of total stellar mass of galaxies and host halo mass, tuned to match the spatial density of galaxies over 0 < z < 2 and the clustering properties at z ∼ 0, is extended to include two different scenarios describing the variation of SFR on M_h. We also present new measurements of the redshift evolution of the average SFR for star-forming galaxies of different stellar masses up to z = 2, using data from the Herschel Multi-tiered Extragalactic Survey for infrared bright galaxies. Combining the EHM with the halo accretion histories from numerical simulations, we trace the stellar mass growth and star-formation history in haloes spanning a range of masses. We find that: (1) the intensity of the star-forming activity in haloes in the probed mass range has steadily decreased from z ∼ 2 to 0; (2) at a given epoch, haloes in the mass range between a few times 10^(11) M_⊙ and a few times 10^(12) M_⊙ are the most efficient at hosting star formation; (3) the peak of SFR density shifts to lower mass haloes over time; and (4) galaxies that are forming stars most actively at z ∼ 2 evolve into quiescent galaxies in today's group environments, strongly supporting previous claims that the most powerful starbursts at z ∼ 2 are progenitors of today's elliptical galaxies.

Additional Information

© 2013 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. Accepted 2013 January 31. Received 2013 January 25; in original form 2012 March 22. First published online: March 7, 2013. We thank the anonymous referee for constructive comments. We also thank Cheng Li for providing the SDSS clustering measurements and the stellar mass function, Rachel Mandelbaum for the stellar mass m∗–halo mass Mh relation from weak lensing, Surhud More for them∗−Mh relation from satellite kinematics, Alexi Leauthaud for the m∗−Mh relation, Samir Salim for the conditional dependence of specific star-formation rate on m∗ in the local Universe, Benjamin Moster for useful discussions on the CSMF, Anthony Lewis for useful discussion on MCMC methods and Peder Norberg for general discussions. LW acknowledges support from UK's Science and Technology Facilities Council grant ST/F002858/1 and an ERC StG grant (DEGAS-259586). SJO is supported by UK's Science and Technology Facilities Council grant ST/F002858/1. The data presented in this paper will be released through the Herschel data base in Marseille HeDaM (hedam.oamp.fr/herMES). SPIRE has been developed by a consortium of institutes led by Cardiff Univ. (UK) and including Univ. Lethbridge (Canada); NAOC (China); CEA, LAM (France); IFSI, Univ. Padua (Italy); IAC (Spain); Stockholm Observatory (Sweden); Imperial College London, RAL, UCL-MSSL, UKATC, Univ. Sussex (UK); and Caltech, JPL, NHSC, Univ. Colorado (USA). This development has been supported by national funding agencies: CSA (Canada); NAOC (China); CEA, CNES, CNRS (France); ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC (UK); and NASA (USA).

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Published - MNRAS-2013-Wang-648-61.pdf


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