论文标题
Z = 6.6的超含量Lyman alpha亮度功能
The Ultraluminous Lyman Alpha Luminosity Function at z=6.6
论文作者
论文摘要
我们在z = 6.6时介绍了超大型LY $α$发射星系（LAE）的光度函数（LF）。我们将超湿的Laes（Ullaes）定义为带有logl（ly $α$）> 43.5 ERG S $^{ - 1} $的星系。我们使用G'，r'，i'，Z'和NB921观察到广阔区域（30 deg $^2 $）的主样本进行选择的主样本，对North Ecliptic Pole（NEP）田地的超弹力板调查。我们选择具有G'，r'，i'> 26，NB921 $ \ leq $ 23.5的候选人和NB921 -z'$ \ leq $ 1.3。使用Keck II上的DEIMOS光谱仪，我们确认我们的14个候选者中的9个为Z = 6.6，其余5个为Z = 6.6的AGN，两个[OIII] $λ$ 5007在z = 0.84和z = 0.85和两个非竞争中发射星系。这强调了对确定准确LFS的全光谱随访的必要性。在Z = 6.6构建Ullae LF时，我们将9个NEP Ullaes与先前发现的两个ullaes结合在一起，并在Cosmos Field中被确认并确认了CR7和COLA1。我们将严格的校正基于模拟而进行不完整。我们将z = 6.6的ullae lf与文献中的z = 5.7和z = 6.6进行比较。我们的数据拒绝了一些以前的LF规范化和权力法指数，但它们与其他LF的标准索引相一致。实际上，对不同文献LF的比较分析表明，没有其他任何一个完全一致，因此，使用在两个红移中以完全相同的方式构造的LFS来确定从z = 5.7到z = 6.6的演变至关重要。
We present the luminosity function (LF) for ultraluminous Ly$α$ emitting galaxies (LAEs) at z = 6.6. We define ultraluminous LAEs (ULLAEs) as galaxies with logL(Ly$α$) > 43.5 erg s$^{-1}$. We select our main sample using the g', r', i', z', and NB921 observations of a wide-area (30 deg$^2$) Hyper Suprime-Cam survey of the North Ecliptic Pole (NEP) field. We select candidates with g', r', i' > 26, NB921 $\leq$ 23.5, and NB921 - z' $\leq$ 1.3. Using the DEIMOS spectrograph on Keck II, we confirm 9 of our 14 candidates as ULLAEs at z = 6.6 and the remaining 5 as an AGN at z = 6.6, two [OIII]$λ$5007 emitting galaxies at z = 0.84 and z = 0.85, and two non-detections. This emphasizes the need for full spectroscopic follow-up to determine accurate LFs. In constructing the ULLAE LF at z = 6.6, we combine our 9 NEP ULLAEs with two previously discovered and confirmed ULLAEs in the COSMOS field: CR7 and COLA1. We apply rigorous corrections for incompleteness based on simulations. We compare our ULLAE LF at z = 6.6 with LFs at z = 5.7 and z = 6.6 from the literature. Our data reject some previous LF normalizations and power law indices, but they are broadly consistent with others. Indeed, a comparative analysis of the different literature LFs suggests that none is fully consistent with any of the others, making it critical to determine the evolution from z = 5.7 to z = 6.6 using LFs constructed in exactly the same way at both redshifts.
