We make publicly available a catalog of calibrated environmental measures for galaxies in the five 3D-HST/CANDELS deep fields .
Leveraging the spectroscopic and grism redshifts from the 3D-HST survey , multi wavelength photometry from CANDELS , and wider field public data for edge corrections , we derive densities in 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 observed galaxies to a mock sample , selected to reproduce the 3D-HST sample selection and redshift accuracy , each 3D-HST galaxy is assigned a probability density function of the host halo mass , and a probability that is a central or a satellite galaxy .
The same procedure is applied to a z = 0 sample selected from SDSS .
We compute the fraction of passive central and satellite galaxies as a function of stellar and halo mass , and redshift , and then derive the fraction of galaxies that were quenched by environment specific processes .
Using the mock sample , we estimate that the timescale for satellite quenching is t _ { quench } \sim 2 - 5 Gyr ; longer at lower stellar mass or lower redshift , but remarkably independent of halo mass .
This indicates that , in the range of environments commonly found within the 3D-HST sample ( M _ { h } \lesssim 10 ^ { 14 } M _ { \odot } ) , satellites are quenched by exhaustion of their gas reservoir in absence of cosmological accretion .
We find that the quenching times can be separated into a delay phase during which satellite galaxies behave similarly to centrals at fixed stellar mass , and a phase where the star formation rate drops rapidly ( \tau _ { f } \sim 0.4 - 0.6 Gyr ) , as shown previously at z = 0 .
We conclude that this scenario requires satellite galaxies to retain a large reservoir of multi-phase gas upon accretion , even at high redshift , and that this gas sustains star formation for the long quenching times observed .