Published in
EDP Sciences, Astronomy & Astrophysics, (581), p. A56, 2015
DOI: 10.1051/0004-6361/201526274
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- [hal-cea.archives-ouvertes.fr] | PDF
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- [www.researchgate.net] | PDF
- [sro.sussex.ac.uk] | PDF
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Satellite content and quenching of star formation in galaxy groups atz~ 1.8
,
M. Béthermin ,
M. Pannella ,
A. Finoguenov,
G. Gozaliasl,
E. Le Floc’h,
C. Schreiber,
V. Strazzullo,
M. Sargent,
T. Wang ,
H. S. Hwang,
F. Valentino,
N. Cappelluti ,
Y. Li
and other authors.
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Abstract
We study the properties of satellites in the environment of massive star-forming galaxies at z ~ 1.8 in the COSMOS field, using a sample of 215 galaxies on the main sequence of star formation with an average mass of ~1011M⊙. At z> 1.5, these galaxies typically trace halos of mass ≳1013M⊙. We use optical-near-infrared photometry to estimate stellar masses and star formation rates (SFR) of centrals and satellites down to ~ 6 × 109M⊙. We stack data around 215 central galaxies to statistically detect their satellite halos, finding an average of ~3 galaxies in excess of the background density. We fit the radial profiles of satellites with simple β-models, and compare their integrated properties to model predictions. We find that the total stellar mass of satellites amounts to ~68% of the central galaxy, while spectral energy distribution modeling and far-infrared photometry consistently show their total SFR to be 25–35% of the central’s rate. We also see significant variation in the specific SFR of satellites within the halo with, in particular, a sharp decrease at