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We analyze the CIII]-1908\AA emission properties in a sample of 3899star-forming galaxies (SFGs) at 2<z<3.8 from the VIMOS Ultra-Deep Survey(VUDS). We find a median EW(CIII])=2.0$\pm$0.2 to 2.2$\pm$0.2\AA ~for the SFGpopulation at 2<z<3 and 3<z<4, resp. About 24% of SFGs are showingEW(CIII])>3\AA, including 20% with 3<EW(CIII])<10\AA ~and 4% with strongemission EW(CIII])>10\AA. A significant fraction of 1.2% of SFGs presentsstrong CIII] emission 20<EW(CIII])<40\AA. This makes CIII] the secondmost-frequent emission line in the UV-rest spectra of SFGs afterLyman-$\alpha$. We find a large dispersion in the weak EW(CIII]) - EW(Ly\alpha)correlation, with galaxies showing strong CIII] and no Ly$\alpha$, andvice-versa. SFGs with 10<EW(CIII])<0\AA ~present strong emission linesincluding CIV-1549, HeII-1640, OIII-1664, but also weaker emission of highlyionized elements SiIV-1403, NIV-1485, NIII-1750, or SiIII-1888, indicating ahard radiation field. We present a broad range of observational evidencesupporting the presence of AGN in the strong CIII] emitting population. AsEW(CIII]) is rising, we identify powerful outflows with velocities up to 1014km/s. The strongest CIII] emitters are preferentially located below the SFGsmain sequence, with the SFR reduced by x2. In addition, the median stellar ageof the strongest emitters is ~0.8 Gyr, three times that of galaxies withEW(CIII])<10\AA. Spectral line analysis presented in a joint paper by Nakajimaet al. (2017) confirms that the strongest emitters require an AGN. We concludethat these properties are indicative of AGN feedback in SFGs at 2<z<3.8,contributing to star-formation quenching. We find that quenching timescales of0.25-0.5x10^9 years are necessary for such AGN feedback to turn part of thestar-forming galaxy population with Mstar>10^10 MSun at z~3 into the populationof quiescent galaxies observed at redshift z~1-2.

The VIMOS Ultra-Deep Survey: evidence for AGN feedback in galaxies with CIII]-$\lambda$1908\AA ~emission 10.8 to 12.5 Gyr ago