Satellite content and quenching of star formation in galaxy groups at z ~ 1.8

Sargent, M, Daddi, E, Béthermin, M, Pannella, M, Finoguenov, A, Gozaliasl, G, Le Floc’h, E, Schreiber, C, Strazzullo, V, Wang, T, Hwang, H S, Valentino, F, Cappelluti, N, Li, Y and Hasinger, G (2015) Satellite content and quenching of star formation in galaxy groups at z ~ 1.8. Astronomy and Astrophysics, 581. ISSN 0004-6361

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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 <100 kpc. After considering different potential explanations, we conclude that this is likely an environmental signature of the hot inner halo. This effect can be explained in the first order by a simple free-fall scenario, suggesting that these low-mass environments can shut down star formation in satellites on relatively short timescales of ~0.3 Gyr.

Item Type: Article
Schools and Departments: School of Mathematical and Physical Sciences > Physics and Astronomy
Subjects: Q Science > QB Astronomy
Depositing User: Mark Sargent
Date Deposited: 09 Feb 2016 08:25
Last Modified: 26 Jan 2018 12:12

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