The brightness of gamma-ray burst (GRB) afterglows and their occurrence in young, blue galaxies make them excellent probes to study star forming regions in the distant Universe. We here elucidate dust extinction properties in the early Universe through the analysis of the afterglows of all known z > 6 GRBs: GRB 090423, 080913 and 050904, at z = 8.2, 6.69, and 6.295, respectively. We gather all available optical and near-infrared photometry, spectroscopy and X-ray data to construct spectral energy distributions (SEDs) at multiple epochs. We then fit the SEDs at all epochs with a dust-attenuated power-law or broken power-law. We find no evidence for dust extinction in GRB 050904 and GRB 090423, with possible evidence for a low level of extinction in GRB 080913. We compare the high redshift GRBs to a sample of lower redshift GRB extinctions and find a lack of even moderately extinguished events (AV ~ 0.3) above z > 4. In spite of the biased selection and small number statistics, this result hints at a decrease in dust content in star-forming environments at high redshifts.
DUSTiER (DUST in the Epoch of Reionization): dusty galaxies in cosmological radiation-hydrodynamical simulations of the Epoch of Reionization with RAMSES-CUDATON
近年来，星际尘埃已成为高红移宇宙和甚高红移宇宙研究中的一个重要课题。证据表明，在再电离时期，大质量恒星形成星系中已经存在高尘埃质量，可能影响电离光子逃逸到星系际介质中。此外，正确估计紫外波长处的尘埃消光对于精确的紫外光度函数（UVLF）预测和解释至关重要。本文研究了尘埃对高红移星系观测性质的影响，以及宇宙再电离。为此，我们耦合的物理模型尘埃生产的完全耦合的辐射流体动力学宇宙学模拟代码RAMSES-CUDATON，并执行$16^3$，$2048^3$，模拟，我们称之为DUSTiER的尘埃在再电离时代。它产生的星系与尘埃质量和紫外线斜率兼容的限制在z $\geq 5$。我们发现，消光对UVLF的亮端有着巨大的影响，甚至早在$\rm z=8$，我们的尘埃UVLF比无尘UVLF更符合观测。在$\rm z=5$中，被遮蔽的恒星形成的比例上升到45%，与ALMA的一些最新结果一致。最后，我们发现尘埃减少了质量比$10^{10} M_\odot$（比$\approx -18$ MAB 1600亮）大的星系的电离光子逃逸> 10%，对于我们最大的星系可能高达80-90%。然而，我们发现电离逃逸分数首先是由星系中的中性氢决定的，因为后者产生的传输比单独通过尘埃小100倍。
Formaldehyde Silhouettes Against the Cosmic Microwave Background: A Mass-Limited, Distance-Independent, Extinction-Free Tracer of Star Formation Across the Epoch of Galaxy Evolution
The THESAN project: Lyman-alpha intensity mapping of cosmic reionization
Center for Astrophysics | Harvard & Smithsonian（哈佛与史密森尼天体物理中心）；Department of Physics, The University of Texas at Dallas（德克萨斯大学达拉斯分校物理系）；Department of Physics and Astronomy, York University（约克大学物理与天文系）；Kavli IPMU (WPI), UTIAS, The University of Tokyo（东京大学卡弗里宇宙物理起源研究所（WPI）、UTIAS）；Department of Physics and Astronomy, University of Pennsylvania（宾夕法尼亚大学物理与天文系）；Department of Physics and Astronomy, Oberlin College（欧柏林学院物理与天文系）；Department of Physics & Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology（麻省理工学院物理系及卡弗里天体物理与空间研究所）
KiDS-DR5: Exploring dust transport in dark matter halos of galaxies
Ruhr University Bochum（鲁尔大学波鸿）；Harvard-Smithsonian Center for Astrophysics（哈佛-史密森天体物理中心）；Center for Astrophysics | Harvard & Smithsonian（天体物理中心 | 哈佛与史密森学会）；Newcastle University（纽卡斯尔大学）；Leiden Observatory, Leiden University（莱顿大学莱顿天文台）
The UV and Ly$α$ Luminosity Functions of galaxies and the Star Formation Rate Density at the end of HI reionization from the VIMOS Ultra-Deep Survey (VUDS)
Haute Ecole Arc Ing\'enierie, University of Applied Sciences \& Arts Western Switzerland (HES-SO), Saint-Imier, Switzerland Département de Physique Théorique；Centre Universitaire d’Informatique, Université de Genève, Genève, Switzerland Nordita, KTH Royal Institute of Technology；Stockholm University, Hannes Alf\'vens v\"ag 12, SE-106 91 Stockholm, Sweden Institute for Particle Physics \& Astrophysics, ETH Zurich, Wolfgang-Pauli-Str 27, 8093 Zurich, Switzerland Laboratoire d’Astrophysique, Ecole Polytechnique Federale de Lausanne EPFL, Observatoire de Sauverny, Versoix 1290, Switzerland Centre for Artificial Intelligence, ZHAW Zurich University of Applied Sciences, Technikumstrasse 71, 8400 Winterthur, Switzerland Institute for Data Science, FHNW University of Applied Sciences \& Arts Northwestern Switzerland, Bahnhofstrasse 6, Windisch, 5210, Switzerland Department of Space, Earth；Environment, Chalmers University of Technology, Onsala Space Observatory, SE-43992 Onsala, Sweden
Homogeneous measurements of proximity zone sizes for 59 quasars in the Epoch of Reionization
Leiden University（莱顿大学）；NSF NOIRLab（美国国家光学红外天文实验室）；University of California, Santa Barbara（加州大学圣塔芭芭拉分校）；Center for Astrophysics | Harvard & Smithsonian（哈佛史密森尼天体物理中心）；Massachusetts Institute of Technology（麻省理工学院）
Exploring the Cosmic Dawn through the 21 cm Forest and High-redshift Radio Sources with the SKA
Max Planck Institute for Astrophysics（马克斯·普朗克天体物理学研究所）；Gifu Shotoku Gakuen University（岐阜女子大学）；Kobayashi Maskawa Institute, Nagoya University（名古屋大学小林益川研究所）；Northeastern University（东北大学）；Liaoning Normal University（辽宁师范大学）；University of Nevada, Las Vegas（内华达大学拉斯维加斯分校）；Yunnan University（云南大学）；Nagoya University（名古屋大学）；Institute for Fundamental Physics of the Universe（宇宙基础物理研究所）；The Institute of Statistical Mathematics（统计数学研究所）；National Astronomical Observatories, Chinese Academy of Sciences（中国科学院国家天文台）；University of Tsukuba（筑波大学）
Dust-UV offsets in high-redshift galaxies in the Cosmic Dawn III simulation
Université de Strasbourg（斯特拉斯堡大学）；CNRS UMR 7550（法国国家科学研究中心 7550联合研究实验室）；Institut d'Astrophysique de Paris（巴黎天体物理学研究所）；UPMC Univ. Paris VI（巴黎第六大学）；The University of Nottingham（诺丁汉大学）；Univ. Lille（里尔大学）；Centrale Lille（里尔中央理工学院）；Universit\'e Paris-Saclay（巴黎萨克雷大学）；Institut d'Astrophysique Spatiale（空间天体物理学研究所）；Leibniz-Institut f\"{u}r Astrophysik（莱布尼茨天体物理研究所）；The University of Texas at Austin（德克萨斯大学奥斯汀分校）；University of Zurich（苏黎世大学）；University of Sussex（萨塞克斯大学）；Chosun University（朝鲜大学）；Lawrence Berkeley National Laboratory（劳伦斯伯克利国家实验室）；Berkeley Center for Cosmological Physics, UC Berkeley（加州大学伯克利分校宇宙学物理中心）；University of Tsukuba（筑波大学）
