# The Grism Lens-Amplified Survey from Space (GLASS). XI. Detection of CIV in Multiple Images of $z=6.11$ Ly$\alpha$ Emitter Behind RXCJ2248.7-4431

## TL;DR

This study reports the first detection of CIV emission in a $z=6.11$ galaxy, providing insights into the ionization state and properties of early galaxies during reionization, using space-based slitless spectroscopy.

## Contribution

It presents the first detection of CIV emission in a high-redshift galaxy at $z=6.11$, offering new constraints on galaxy ionization and metallicity during reionization.

## Key findings

- CIV emission detected at 3-5σ in two images of the galaxy.
- No significant CIII] emission detected, with EW<20Å.
- Galaxy has a young stellar population, high ionization, and low metallicity.

## Abstract

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$\lambda\lambda$1548,1551\AA\ in \HST\ slitless grism spectroscopy obtained by GLASS of a Ly$\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]$\lambda\lambda$1907,1909\AA\ emission implying an equivalent width EW$_\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$1640\AA\ emission line and the OIII]$\lambda\lambda$1661,1666\AA\ doublet, we put constraints on the metallicity and the ionization state of the galaxy. The estimated line ratios and equivalent widths do not support a scenario where an AGN is responsible for ionizing the carbon atoms. SED fits including nebular emission lines imply a source with a mass of log(M/M$_\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.