The CIII] and CIV rest-frame UV emission lines are powerful probes of the ionizations states of galaxies. They have furthermore been suggested as alternatives for spectroscopic redshift confirmation of objects at the epoch of reionization ($z>6$), where the most frequently used redshift indicator, Ly$alpha$, is attenuated by the high fraction of neutral hydrogen in the inter-galactic medium. However, currently only very few confirmations of carbon UV lines at these high redshifts exist, making it challenging to quantify these claims. Here, we present the detection of CIV$lambdalambda$1548,1551AA in HST slitless grism spectroscopy obtained by GLASS of a Ly$alpha$ emitter at $z=6.11$ multiply imaged by the massive foreground galaxy cluster RXJ2248. The CIV emission is detected at the 3--5$sigma$ level in two images of the source, with marginal detection in two other images. We do not detect significant CIII]$lambdalambda$1907,1909AA emission implying an equivalent width EW$_textrm{CIII]}<20$AA (1$sigma$) and $textrm{CIV/CIII}>0.7$ (2$sigma$). Combined with limits on the rest-frame UV flux from the HeII$lambda$1640AA emission line and the OIII]$lambdalambda$1661,1666AA doublet, we put constraints on the metallicity and the ionization state of the galaxy. The estimated line ratios and equivalent widths do not support a scenario where an AGN is responsible for ionizing the carbon atoms. SED fits including nebular emission lines imply a source with a mass of log(M/M$_odot)sim9$, SFR of around 10M$_odot$/yr, and a young stellar population $<50$Myr old. The source shows a stronger ionizing radiation field than objects with detected CIV emission at $z<2$ and adds to the growing sample of low-mass (log(M/M$_odot)lesssim9$) galaxies at the epoch of reionization with strong radiation fields from star formation.
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