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We study the properties of satellites in the environment of massivestar-forming galaxies at z~1.8 in the COSMOS field, using a sample of 215galaxies on the main sequence of star formation with an average mass of 10^11Msun. At z>1.5, these galaxies typically trace halos of mass >10^13 Msun. Weuse optical-near-infrared photometry to estimate stellar masses and starformation rates (SFR) of centrals and satellites down to ~6*10^9 Msun. We stackdata around 215 central galaxies to statistically detect their satellite halos,finding an average of ~3 galaxies in excess of the background density. We fitthe radial profiles of satellites with simple beta-models, and compare theirintegrated properties to model predictions. We find that the total stellar massof satellites amounts to 68% of the central galaxy, while SED modeling andfar-infrared photometry consistently show their total SFR to be 25-35% of thecentral's rate. We also see significant variation in the specific SFR ofsatellites within the halo with, in particular, a sharp decrease at <100 kpc.After considering different potential explanations, we conclude that this islikely an environmental signature of the hot inner halo. This effect can beexplained in the first order by a simple free-fall scenario, suggesting thatthese low-mass environments can shut down star formation in satellites onrelatively short timescales of ~0.3 Gyr.

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