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We used the Space Telescope Imaging Spectrograph (STIS) on the Hubble SpaceTelescope (HST) to observe the semi-forbidden CIII] emission in Green Peagalaxies at 0.13 < z < 0.3. We detect CIII] emission in 7/10 galaxies withCIII] equivalent widths that range from 2-10\AA~. The observed CIII] emissionline strengths are consistent with the predictions from photoionization modelswhich incorporate the effects of binary stellar evolution with young stellarages < 3-5 Myrs, and high ionization parameters (logU > -2). The hard ionizingradiation from young massive stars, and high nebular temperatures atlow-metallicities can account for the observed high equivalent widths of CIII]and [OIII] emission lines. The Green Pea galaxies do not show a significantcorrelation between the Ly$\alpha$ and CIII] equivalent widths, and theobserved scatter is likely due to the variations in the optical depth ofLy$\alpha$ to the neutral gas. Green Pea galaxies are likely to bedensity-bounded, and we examined the dependence of CIII] emission on the Lymancontinuum optical depth. The potential LyC leaker galaxies in our sample havehigh CIII] equivalent widths that can only be reproduced by starburst ages asyoung as < 3 Myrs and harder ionizing spectra than the non-leakers. Among thegalaxies with similar metallicities and ionization parameters, the CIII]equivalent width appears to be stronger for those with higher optical depth toLyC, as expected from the photoionization models. Further investigation of alarger sample of CIII]-emitters is necessary to calibrate the dependence ofCIII] emission on the escape of LyC radiation, and to enable application of theCIII] diagnostics to galaxies in the reionization epoch.

The Semi-forbidden CIII]$\lambda$1909\AA~ Emission in the Rest-Ultraviolet Spectra of Green Pea Galaxies