Texas Spectroscopic Search for Ly$α$ Emission at the End of Reionization III. the Ly$α$ Equivalent-width Distribution and Ionized Structures at $z > 7$
Intae Jung, Steven L. Finkelstein, Mark Dickinson, Taylor A. Hutchison, Rebecca L. Larson, Casey Papovich, Laura Pentericci, Amber N. Straughn, Yicheng Guo, San… 展开作者
Intae Jung, Steven L. Finkelstein, Mark Dickinson, Taylor A. Hutchison, Rebecca L. Larson, Casey Papovich, Laura Pentericci, Amber N. Straughn, Yicheng Guo, Sangeeta Malhotra, James Rhoads, Mimi Song, Vithal Tilvi, Isak Wold
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Published 2020 November 27 in ApJ. Changed to match the published version (HI fraction & Figure 12 updated and other minor changes). 27 pages, 15 figures, 3 tables
Ly$α$ emission from galaxies can be utilized to characterize the ionization state in the intergalactic medium (IGM). We report our search for Ly$α$ emission at $z>7$ using a comprehensive Keck/MOSFIRE near-infrared spectroscopic dataset, as part of the Texas Spectroscopic Search for Ly$α$ Emission at the End of Reionization Survey. We analyze data from 10 nights of MOSFIRE observations which together target 72 high-$z$ candidate galaxies in the GOODS-N field, all with deep exposure times of 4.5-19 hr. Utilizing an improved automated emission-line search, we report 10 Ly$α$ emission lines detected ($>$4$σ$) at $z>7$, significantly increasing the spectroscopically confirmed sample. Our sample includes large equivalent-width (EW) Ly$α$ emitters ($>$50Å), and additional tentative Ly$α$ emission lines detected at 3 - 4$σ$ from five additional galaxies. We constrain the Ly$α$ EW distribution at $z\sim7.6$, finding a significant drop from $z\lesssim6$, suggesting an increasing fraction of neutral hydrogen (HI) in the IGM in this epoch. We estimate the Ly$α$ transmission through the IGM ($=$EW$_{z\sim\text{7.6}}$/EW$_{z\sim\text{2-6}}$), and infer an IGM HI fraction ($X_{\text{HI}}$) of $49^{+19}_{-19}\%$ at $z\sim7.6$, which is lower in modest tension ($>$1$σ$) with recent measurements at $z \sim$ 7.6. The spatial distribution of the detected Ly$α$ emitters implies the presence of a potential highly ionized region at $z\sim7.55$ which hosts four Ly$α$ emitters within a $\sim$ 40 cMpc spatial separation. The prominence of this ionized region in our dataset could explain our lower inferred value of $X_{\text{HI}}$, though our analysis is also sensitive to the chosen reference Ly$α$ EW distribution values and reionization models.
Deep JWST spectroscopy of galaxies in a candidate ionized bubble at $z = 8.7$: probing reionization at pMpc scales with Ly$α$ emission
University of Cambridge（剑桥大学）；University of Arizona（亚利桑那大学）；Niels Bohr Institute, University of Copenhagen（哥本哈根大学尼尔斯·玻尔研究所）；University of California, Santa Barbara（加州大学圣塔芭芭拉分校）；University of Vienna（维也纳大学）
The THESAN project: Lyman-alpha emitters as probes of ionized bubble sizes
Massachusetts Institute of Technology（麻省理工学院）；The University of Texas at Dallas（德克萨斯大学达拉斯分校）；Universidad ECCI（ECCI大学）；York University（约克大学）；The University of Tokyo（东京大学）；University of Edinburgh（爱丁堡大学）
Influence of the Spectral Energy Distribution of Reionization-Era Sources on the Lyman-$α$ Forest
Ludwig-Maximilians-Universität München (LMU)（慕尼黑路德维希-马克西米利安大学）；Univ Lyon, Univ Lyon1, Ens de Lyon, CNRS, CRAL UMR5574（里昂大学，里昂第一大学，巴黎高等师范学校里昂分校，法国国家科学研究中心，CRAL）；School of Physics and Astronomy, University of Nottingham（诺丁汉大学物理与天文学学院）；SISSA - International School for Advanced Studies（国际高等研究学院）；INFN – National Institute for Nuclear Physics（意大利国家核物理研究所）；IFPU, Institute for Fundamental Physics of the Universe（宇宙基础物理研究所）；INAF, Osservatorio Astronomico di Trieste（的里雅斯特天文台）；ICSC - Centro Nazionale di Ricerca in High Performance Computing, Big Data e Quantum Computing（高性能计算、大数据和量子计算国家研究中心）；Kavli IPMU (WPI), UTIAS, The University of Tokyo（东京大学 Kavli 宇宙粒子与宇宙学研究所）；Center for Data-Driven Discovery, Kavli IPMU (WPI), UTIAS, The University of Tokyo（数据驱动发现中心）
Galaxy Protoclusters as Drivers of Cosmic Reionization: I. Bubble Overlap at Redshift z ~ 7 in LAGER-z7OD1
University of California Santa Barbara（加州大学圣塔芭芭拉分校）；Goddard Space Flight Center（戈达德太空飞行中心）；The University of Tokyo（东京大学）；Space Telescope Science Institute（太空望远镜科学研究所）；MIT Kavli Institute for Astrophysics and Space Research（麻省理工学院卡弗里天体物理学与空间研究研究所）；CNRS, Institut d'Astrophysique de Paris（法国国家科学研究中心，巴黎天体物理研究所）；Chinese Academy of Sciences（中国科学院）；University of Science and Technology of China（中国科学技术大学）
Bubble mapping with the Square Kilometer Array -- I. Detecting galaxies with Euclid, JWST, WFIRST and ELT within ionized bubbles in the intergalactic medium at z>6
Probing the thermal history during reionization using a semi-numerical photon-conserving code SCRIPT
星系际介质（IGM）在再电离时期的电离和热状态一直是最近的兴趣，因为它们与第一批恒星的密切联系。我们在本文中提出了一个半数值代码，计算大规模的温度和电离氢场在宇宙学上的代表性体积占补丁在这些数量所产生的再电离。该代码是对先前开发的用于研究电离区域生长的版本的扩展，即光子守恒的再电离半数值代码（Semi Numerical Code for Reionization with Photon Conservation，缩写为WNTT）。在本版本中的主要补充是非均匀重组，这是必不可少的温度计算。这种扩展版本的RECT还实现了再电离期间光加热的物理后果，例如，辐射反馈这些增强功能使我们能够预测早期版本不可行的观测值。其中包括星系的紫外光度函数的暗端（这可能受到辐射反馈的影响）和低密度IGM在$z\sim 6$的温度-密度关系。我们研究了不同的自由参数和处方我们的模型上的各种可观的效果。我们的分析的结论是，它应该是可能的，把约束的IGM的热和电离状态的演化使用现有的观测占所有可能的变化的自由参数。参数空间的详细探索将在未来进行。
JWST ASPIRE: How Did Galaxies Complete Reionization? Evidence for Excess IGM Transmission around ${\rm [O\,{\scriptstyle III}]}$ Emitters during Reionization
The Lumina Project: Morphology of Ionized Bubbles and Neutral Islands
Massachusetts Institute of Technology（麻省理工学院）；The University of Texas at Dallas（德克萨斯大学达拉斯分校）；Philipps Universität Marburg（马尔堡菲利普斯大学）；Max Planck Institute for Astrophysics（马克斯·普朗克天体物理研究所）；York University（约克大学）
