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Recently, the CIII] and CIV emission lines have been observed in galaxies inthe early Universe ($z>5$), providing new ways to measure their redshift andstudy their stellar populations and AGN. We explore the first blind CII], CIII]and CIV survey ($z\sim0.68, 1.05, 1.53$, respectively) presented in Stroe etal. (2017). We derive luminosity functions (LF) and study properties of CII],CIII] and CIV line emitters through comparisons to the LFs of H$\alpha$ andLy$\alpha$ emitters, UV selected star forming (SF) galaxies and quasars atsimilar redshifts. The CII] LF at $z\sim0.68$ is equally well described by aSchechter or a power-law LF, characteristic of a mixture of SF and AGNactivity. The CIII] LF ($z\sim1.05$) is consistent to a scaled down version ofthe Schechter H$\alpha$ and Ly$\alpha$ LF at their redshift, indicating a SForigin. In stark contrast, the CIV LF at $z\sim1.53$ is well fit by apower-law, quasar-like LF. We find that the brightest UV sources ($M_{UV}<-22$)will universally have CIII] and CIV emission. However, on average, CIII] andCIV are not as abundant as H$\alpha$ or Ly$\alpha$ emitters at the sameredshift, with cosmic average ratios of $\sim0.02-0.06$ to H$\alpha$ and$\sim0.01-0.1$ to intrinsic Ly$\alpha$. We predict that the CIII] and CIV linescan only be truly competitive in confirming high redshift candidates when thehosts are intrinsically bright and the effective Ly$\alpha$ escape fraction isbelow 1 per cent. While CIII] and CIV were proposed as good tracers of young,relatively low-metallicity galaxies typical of the early Universe, we findthat, at least at $z\sim1.5$, CIV is exclusively hosted by AGN/quasars,especially at large line equivalent widths.

A ${\bf 1.4}$ deg${\bf ^2}$ blind survey for CII], CIII] and CIV at ${\bf z\sim0.7-1.5}$. II: luminosity functions and cosmic average line ratios