Deep spectroscopy of galaxies in the reionization-era has revealed intense CIII] and CIV line emission (EW $>15-20$ A). In order to interpret the nebular emission emerging at $z>6$, we have begun targeting rest-frame UV emission lines in galaxies with large specific star formation rates (sSFRs) at $1.3 6$ only in large sSFR galaxies with [OIII]+H$\beta$ EW $>1500$ A. In contrast to previous studies, we find that many galaxies with intense [OIII] have weak CIII] emission (EW $=5-8$ A), suggesting that the radiation field associated with young stellar populations is not sufficient to power strong CIII]. Photoionization models demonstrate that the spread in CIII] among systems with large sSFRs ([OIII]+H$\beta$ EW $>1500$ A) is driven by variations in metallicity, a result of the extreme sensitivity of CIII] to electron temperature. We find that the strong CIII] emission seen at $z>6$ (EW $>15$ A) requires metal poor gas ($\simeq0.1\ Z_\odot$) whereas the weaker CIII] emission in our sample tends to be found at moderate metallicities ($\simeq0.3\ Z_\odot$). The luminosity distribution of the CIII] emitters in our $z\simeq1-3$ sample presents a consistent picture, with stronger emission generally linked to low luminosity systems ($M_{\rm{UV}}>-19.5$) where low metallicities are more likely. We quantify the fraction of strong CIII] and CIV emitters at $z\simeq1-3$, providing a baseline for comparison against $z>6$ samples. We suggest that the first UV line detections at $z>6$ can be explained if a significant fraction of the early galaxy population is found at large sSFR ($>200$ Gyr$^{-1}$) and low metallicity ($<0.1\ Z_\odot$).

中文翻译：

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1.3 < z < 3.7 处极端 [OIII] 发射器的静止帧紫外光谱：迈向 JWST 的高红移紫外参考样品

再电离时代星系的深度光谱揭示了强烈的 CIII] 和 CIV 线发射（EW $>15-20 $ A）。为了解释在 $z>6$ 处出现的星云发射，我们已经开始针对具有大比恒星形成率 (sSFR) 的星系中的静止帧 UV 发射线为 $1.3 6$ 仅在具有 [OIII]+ 的大型 sSFR 星系中H$\beta$ EW $>1500$ A. 与之前的研究相比，我们发现许多 [OIII] 强的星系具有弱的 CIII] 发射（EW $=5-8$ A），这表明辐射场相关年轻的恒星数量不足以为强大的 CIII 提供动力]。光电离模型表明，CIII] 在具有大 sSFR（[OIII]+H$\beta$EW $>1500$A）的系统中的扩散是由金属丰度的变化驱动的，这是 CIII] 对电子温度极端敏感的结果. 我们发现在 $z>6$ (EW $>15$ A) 处看到的强 CIII] 排放需要贫金属气体 ($\simeq0.1\ Z_\odot$) 而我们样本中较弱的 CIII] 排放倾向于可在中等金属度 ($\simeq0.3\Z_\odot$) 中找到。我们的 $z\simeq1-3$ 样本中 CIII] 发射器的光度分布呈现出一致的图像，更强的发射通常与低金属度的低光度系统 ($M_{\rm{UV}}>-19.5$) 有关更有可能。我们在 $z\simeq1-3$ 处量化了强 CIII] 和 CIV 发射器的比例，为与 $z>6$ 样本进行比较提供了基线。我们认为，如果在大 sSFR（$>200$ Gyr$^{-1}$）和低金属丰度（$ <0.1\ Z_\dot$)。