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We make publicly available a catalog of calibrated environmental measures forgalaxies in the five 3D-HST/CANDELS deep fields. Leveraging the spectroscopicand grism redshifts from the 3D-HST survey, multi wavelength photometry fromCANDELS, and wider field public data for edge corrections, we derive densitiesin fixed apertures to characterize the environment of galaxies brighter than$JH_{140} < 24$ mag in the redshift range $0.5<z<3.0$. By linking observedgalaxies to a mock sample, selected to reproduce the 3D-HST sample selectionand redshift accuracy, each 3D-HST galaxy is assigned a probability densityfunction of the host halo mass, and a probability that is a central or asatellite galaxy. The same procedure is applied to a $z=0$ sample selected fromSDSS. We compute the fraction of passive central and satellite galaxies as afunction of stellar and halo mass, and redshift, and then derive the fractionof galaxies that were quenched by environment specific processes. Using themock sample, we estimate that the timescale for satellite quenching is $t_{\rmquench} \sim 2-5$ Gyr; longer at lower stellar mass or lower redshift, butremarkably independent of halo mass. This indicates that, in the range ofenvironments commonly found within the 3D-HST sample, satellites are quenchedby exhaustion of their gas reservoir in absence of cosmological accretion. Wefind that the quenching times can be separated into a delay phase during whichsatellite galaxies behave similarly to centrals at fixed stellar mass, and aphase where the star formation rate drops rapidly ($\sim 0.4-0.6$ Gyr), asshown previously at $z=0$. We conclude that this scenario requires satellitegalaxies to retain a large reservoir of multi-phase gas upon accretion, even athigh redshift, and that this gas sustains star formation for the long quenchingtimes observed.

Galaxy environment in the 3D-HST fields. Witnessing the onset of satellite quenching at z ~ 1-2