空间棱镜透镜放大巡天（GLASS）。XI。在RXCJ2248后面的$z=6.11$和$α$的多个图像中检测CIV。7 - 4431
The Grism Lens-Amplified Survey from Space (GLASS). XI. Detection of CIV in Multiple Images of $z=6.11$ Ly$α$ Emitter Behind RXCJ2248.7-4431
摘要：
CIII]和CIV静止系紫外发射线是探测星系电离态的有力工具。此外，它们还被建议作为在再电离时期（$z>6$）光谱红移确认对象的替代品，其中最常用的红移指示剂Ly $z>6$被银河系间介质中的高比例中性氢衰减。然而，目前只有极少数确认碳紫外线在这些高红移存在，使其具有挑战性的量化这些索赔。在这里，我们提出了在\HST\无狭缝棱镜光谱中探测到CIV $λλ$ 1548，1551的方法，该方法是通过对$z=6.11$上的Ly $α$发射体进行玻璃散射，并由大质量前景星系团RXJ 2248多次成像。在源的两个图像中，在3 - 5 $σ$水平上检测CIV发射，在另外两个图像中进行边缘检测。我们没有检测到显著的CIII] $λλ$ 1907，1909发射，这意味着等效宽度EW $_\textrm{CIII]}<20$ E1（1 PDMATHAMR）和$\textrm{CIV/CIII}>0.7$（2 PDMATHAMR）。结合HeII $λ$ 1640 <$E发射线和OIII] $λλ$ 1661，1666 <$E双重谱线的静止坐标系UV通量的限制，我们对银河系的金属丰度和电离态施加了限制。估计的谱线比和等效宽度不支持活动星系核负责电离碳原子的假设。包括星云发射线的SED拟合意味着一个质量为log（M/M $_\odot)\sim9$，SFR约为10M $_\odot$/yr的源，以及一个年轻的恒星群$<50$ Myr。该源显示出比在$z<2$检测到CIV发射的物体更强的电离辐射场，并增加了不断增长的低质量（log（M/M $_\odot)\lesssim9$）星系的样本，在再电离的时代，从恒星形成的强辐射场。
英文摘要：
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$α$, 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$λλ$1548,1551Å in \HST\ slitless grism spectroscopy obtained by GLASS of a Ly$α$ emitter at $z=6.11$ multiply imaged by the massive foreground galaxy cluster RXJ2248. The CIV emission is detected at the 3--5$σ$ level in two images of the source, with marginal detection in two other images. We do not detect significant CIII]$λλ$1907,1909Å emission implying an equivalent width EW$_\textrm{CIII]}<20$Å (1$σ$) and $\textrm{CIV/CIII}>0.7$ (2$σ$). Combined with limits on the rest-frame UV flux from the HeII$λ$1640Å emission line and the OIII]$λλ$1661,1666Å doublet, we put constraints on the metallicity and the ionization state of the galaxy. The estimated line ratios and equivalent widths do not support a scenario where an AGN is responsible for ionizing the carbon atoms. SED fits including nebular emission lines imply a source with a mass of log(M/M$_\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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