  We explore how the group environment may affect the evolution of star-forming
galaxies. We select 1197 Galaxy And Mass Assembly (GAMA) groups at $0.05\leq z
\leq 0.2$ and analyze the projected phase space (PPS) diagram, i.e. the galaxy
velocity as a function of projected group-centric radius, as a local
environmental metric in the low-mass halo regime $10^{12}\leq
(M_{200}/M_{\odot})< 10^{14}$. We study the properties of star-forming group
galaxies, exploring the correlation of star formation rate (SFR) with radial
distance and stellar mass. We find that the fraction of star-forming group
members is higher in the PPS regions dominated by recently accreted galaxies,
whereas passive galaxies dominate the virialized regions. We observe a small
decline in specific SFR of star-forming galaxies towards the group center by a
factor $\sim 1.2$ with respect to field galaxies. Similar to cluster studies,
we conclude for low-mass halos that star-forming group galaxies represent an
infalling population from the field to the halo and show suppressed star
formation.
