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Deep spectroscopy of galaxies in the reionization-era has revealed intenseCIII] and CIV line emission (EW $>15-20$ \r{A}). In order to interpret thenebular emission emerging at $z>6$, we have begun targeting rest-frame UVemission lines in galaxies with large specific star formation rates (sSFRs) at$1.3<z<3.7$. We find that CIII] reaches the EWs seen at $z>6$ only in largesSFR galaxies with [OIII]+H$\beta$ EW $>1500$ \r{A}. In contrast to previousstudies, we find that many galaxies with intense [OIII] have weak CIII]emission (EW $=5-8$ \r{A}), suggesting that the radiation field associated withyoung stellar populations is not sufficient to power strong CIII].Photoionization models demonstrate that the spread in CIII] among systems withlarge sSFRs ([OIII]+H$\beta$ EW $>1500$ \r{A}) is driven by variations inmetallicity, a result of the extreme sensitivity of CIII] to electrontemperature. We find that the strong CIII] emission seen at $z>6$ (EW $>15$\r{A}) requires metal poor gas ($\simeq0.1\ Z_\odot$) whereas the weaker CIII]emission in our sample tends to be found at moderate metallicities ($\simeq0.3\Z_\odot$). The luminosity distribution of the CIII] emitters in our$z\simeq1-3$ sample presents a consistent picture, with stronger emissiongenerally linked to low luminosity systems ($M_{\rm{UV}}>-19.5$) where lowmetallicities are more likely. We quantify the fraction of strong CIII] and CIVemitters at $z\simeq1-3$, providing a baseline for comparison against $z>6$samples. We suggest that the first UV line detections at $z>6$ can be explainedif a significant fraction of the early galaxy population is found at large sSFR($>200$ Gyr$^{-1}$) and low metallicity ($<0.1\ Z_\odot$).

Rest-frame UV spectroscopy of extreme [OIII] emitters at $1.3