field counterpart, consistent with many cluster studies [@vul10; @hai13; @alb14]. The excess of the quiescent fraction in clusters compared to that in the field galaxies reveals a positive correlation with the stellar mass similar to the trend of the mass-dependent environment quenching in the strangulation model introduced by [@font08]. It is thus concluded that the quenching mechanism of strangulation appears to fit better the observed trend better.

It is known that an evolutionary sequence of star formation is likely related to radial gradients through the dynamical friction, which causes the correlation between satellite radius and infall time [@gao04]. Hence galaxy properties as a function of the radius can provide us with hints of the relative importance of different quenching processes that halt star formation in a dense environment, and further help our understanding of galaxy formation and evolution. We hence extend our previous results to include the discussion of galaxy properties in terms of the projected group-centric radius $r_p$ and aim to understand at which radius the possible quenching mechanisms acting on galaxies effectively alter galaxy properties. This work is based on the same group catalog of two PS1 medium-deep fields, MD04 and MD07, produced by the probability friends-of-friends (or 