Distribution of CIII] emitters with different EW(CIII]) in the M_star–SFR plane. The CIII] emitters with different EW are identified by the differently colored symbols. The parent sample of star-forming galaxies at redshifts 2 <  z <  3.8 in VUDS is identified as gray symbols whose distribution is identified by the contours, and the main sequence of VUDS galaxies at z  ∼  3 is indicated by black open squares that are connected by a thick line. We note that both the strong and very strong CIII] emitters are on average below the MS, with median values identified by the connected orange and red squares, respectively. The lower SFR of these strong CIII] emitters compared to the MS is possibly caused by a strong star formation quenching produced by AGN feedback in the host star-forming galaxies.