http://arxiv.org/abs/1702.04731
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 (EoR), 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 $z>6$ 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 3-5$\sigma$ in two images of the source. We do not detect significant CIII] 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 constrain the metallicity and the ionization state of the galaxy. The emission line flux ratios reveal a galaxy with an ionization parameter $\log U\gtrsim-2.5$ arising from star formation with a metallicity of $\gtrsim0.02\textrm{Z}_\odot$. The estimated line ratios and EWs 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 50M$_\odot$/yr, and a young stellar population $<50$Myr old. Hence, this 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 EoR with extreme radiation fields from star formation.
K. Schmidt, K. Huang, T. Treu, et. al.
Fri, 17 Feb 17
7/43
Comments: 18 pages, 8 figures, 3 tables, submitted to ApJ
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