Clump-Scale Dust Attenuation in Epoch of Reionization Galaxies: Spatially Resolved Properties from FirstLight Simulations
Center for Computational Astrophysics, Flatiron Institute（平顿研究所计算天体物理中心）；Department of Physics, The University of Tokyo（东京大学物理学系）；Sterrenkundig Observatorium Department of Physics and Astronomy Universiteit Gent（根特大学物理与天文系天文观测台）；Waseda Research Institute for Science and Engineering, Faculty of Science and Engineering, Waseda University（早稻田大学理工学学术院理工学研究科）；Department of Physics, School of Advanced Science and Engineering, Faculty of Science and Engineering, Waseda University（早稻田大学理工学学术院先进理工学部物理学系）；Departamento de Fisica Teorica and CIAFF, Facultad de Ciencias, Universidad Autonoma de Madrid（马德里自治大学理学院理论物理系及CIAFF）；CIAFF, Facultad de Ciencias, Universidad Autonoma de Madrid（马德里自治大学理学院CIAFF）；Department of Physics, Graduate School of Science, Kyoto University（京都大学理学研究科物理学系）；Theoretical Astrophysics, Department of Earth and Space Science, The University of Osaka（大阪大学地球空间科学系理论天体物理学）
Yurina Nakazato, Kosei Matsumoto, Akio K. Inoue, Daniel Ceverino, Takashi Hosokawa, Daisuke Toyouchi
备注：
23 pages including appendices (15 pages main text), 8 figures, accepted to ApJ
Understanding dust attenuation in galaxies at both integrated and spatially resolved scales is fundamental for accurately determining the physical properties of galaxies. Recent high-spatial-resolution observations with ALMA and JWST enable investigations of spatially resolved properties in high-redshift galaxies ($z \gtrsim 6$), but spatial variations in dust observables remain poorly constrained. We use cosmological zoom-in simulations combined with post-processing dust radiative transfer calculations for 376 clumpy galaxies at $z=6$-$9$ with stellar masses of $M_* \gtrsim 10^9 \, M_\odot$. For each system, we investigate dust attenuation and re-emission properties for three components: system-integrated, individual clumps, and diffuse regions. We find that system-integrated attenuation curves are grayer than the Calzetti curve, even when assuming MW- or SMC-type dust. Attenuation curves of individual clumps are even grayer, while diffuse regions exhibit steeper curves owing to enhanced scattering in optically thin environments. Since the effects of optical depth and dust-star geometry are intrinsically degenerate in attenuation curves, we introduce a toy model based on the IRX-$Δβ$ plane, where $Δβ$ denotes the difference between attenuated and intrinsic UV slopes. Applying this framework, we find that clumps have dust column densities approximately an order of magnitude higher than system-integrated values and exhibit co-spatial or dust-extended geometries. In contrast, system-integrated attenuation reflects star-extended geometries driven by contributions from optically thin diffuse regions. We apply this framework to REBELS-IFU galaxies at $z \sim 7$ and find good agreement with our simulation predictions.
A merger-driven scenario for clumpy galaxy formation in the epoch of reionization: Physical properties of clumps in the FirstLight simulation
The University of Tokyo（东京大学）；Kavli Institute for the Physics and Mathematics of the Universe (WPI), UT Institute for Advanced Study, The University of Tokyo（宇宙物理与数学 Kavli 研究所（WPI），UT 高等研究院，东京大学）；Research Center for the Early Universe, School of Science, The University of Tokyo（东京大学理学部早期宇宙研究中心）
Accelerated size evolution in the FirstLight simulations from z=14 to z=5
Universidad Autonoma de Madrid（马德里自治大学）；Flatiron Institute（平顿研究所）；The University of Tokyo（东京大学）；Kavli Institute for the Physics and Mathematics of the Universe (WPI), UT Institute for Advanced Study, The University of Tokyo（东京大学宇宙研究前沿机构 Kavli宇宙物理与数学研究所（WPI））；Research Center for the Early Universe, School of Science, The University of Tokyo（东京大学理学部宇宙早期研究中心）；Universität Heidelberg（海德堡大学）；Centro de Astrobiología (CAB), CSIC-INTA（西班牙国家天文生物研究中心 (CAB)，CSIC-INTA）
Improving photometric redshifts of Epoch of Reionization galaxies: a new empirical transmission curve with neutral hydrogen damping wing Ly$α$ absorption
Reionization and the ISM/Stellar Origins with JWST and ALMA (RIOJA): The core of the highest redshift galaxy overdensity at $z = 7.88$ confirmed by NIRSpec/JWST
Resolving dust and Lyα emission in a lensed galaxy at the epoch of reionization with JWST/CANUCS
University of Ljubljana（卢布尔雅那大学）；University of California Davis（加州大学戴维斯分校）；Arizona State University（亚利桑那州立大学）；University of Groningen（格罗宁根大学）；INAF - Osservatorio Astronomico di Roma（意大利国家天体物理研究所罗马天文台）；Saint Mary’s University（圣玛丽大学）；Space Telescope Science Institute（太空望远镜科学研究所）
SED Analysis of 13 Spectroscopically Confirmed Galaxies at z$\simeq$6 to Constrain UV-Slope, Model Dust Attenuation and Escape Fractions
宇宙中氢的再电离被认为是通过红移$z\simeq5.5-6$完成的。为了探索这个时代，斯巴鲁深场（SDF）的星系观测已经在$z\simeq6$确定了100多个星系，其中许多通过后续观测得到了光谱学的证实。我们用CIGALE和Dense Basis代码模拟了13个SDF星系的光谱能量分布（SED）。模拟深红外测光有可能限制星系的莱曼连续（LyC）逃逸分数（\fesc）。我们使用模拟的星云发射线，并发现隐含的逃逸分数范围从\textbf{0 to 0.8 with a median of $\sim$0.35 for Dense Basis and $\sim$0.55 for CIGALE.}数据中存在显着的不确定性，使拟合结果在一个大范围的\fesc \为个别对象。这意味着星系的\fesc -值可能足够高，足以完成$z\sim6$的再电离。此外，我们没有发现强的趋势之间的UV斜率$β$或\EBminV与模型\fesc。如果是真的，缺乏趋势表明，除了星云发射或尘埃灭绝之外，其他因素可能导致LyC逃逸，例如在ISM中存在的洞具有足够宽的开口角度，来自超新星和/或弱AGN的流出，导致一系列隐含的\fesc -值取决于每个星系的视角。目前的\textit{HST, Spitzer}和基于地面的光度和星系模型的误差仍然很大，因此需要用\textit{James Webb Space Tele…
Dark-ages Reionization and Galaxy Formation Simulation XX. The Ly$α$ IGM transmission properties and environment of bright galaxies during the Epoch of Reionization
Dark-ages Reionization and Galaxy Formation Simulation -- XIX: Predictions of infrared excess and cosmic star formation rate density from UV observations
The gradual decline of Ly$α$ visibility in the CANDELS fields: evidence for the combined effects of galaxy evolution and reionization
INAF – Osservatorio Astronomico di Roma（意大利国家天体物理研究所罗马天文台）；Scuola Normale Superiore（比萨高等师范学院）；NSF’s National Optical-Infrared Astronomy Research Laboratory（美国国家光学红外天文研究实验室）；Department of Astronomy, The University of Texas at Austin（德克萨斯大学奥斯汀分校天文学系）；Cosmic Frontier Center, The University of Texas at Austin（德克萨斯大学奥斯汀分校宇宙前沿中心）；Armagh Observatory and Planetarium（阿马赫天文馆与天文台）；Institute for Astronomy, University of Edinburgh（爱丁堡大学天体物理研究所）；Astrophysics Science Division, NASA Goddard Space Flight Center（NASA戈达德太空飞行中心天体物理学部）；Center for Space Sciences and Technology, UMBC（马里兰大学巴尔的摩分校空间科学与技术中心）
REBELS-IFU: Spatially Resolved Ionizing Photon Production Efficiencies of 12 Bright Galaxies in the Epoch of Reionization
Universitat de València（瓦伦西亚大学）；Instituto de Física de Cantabria（坎塔布里亚物理研究所）；Academia Sinica（中央研究院）；Universidad Diego Portales（迭戈·波特莱斯大学）；Leiden University（莱顿大学）；The University of Manchester（曼彻斯特大学）；University of Western Australia（西澳大利亚大学）
High Resolution HST Imaging Survey of Local Star-Forming Galaxies I: Spatially-Resolved Obscured Star Formation with H$α$ and Paschen-$β$ Recombination Lines
NIRSpec View of the Appearance and Evolution of Balmer Breaks and the Transition from Bursty to Smooth Star Formation Histories from Deep Within the Epoch of Reionization to Cosmic Noon
First Spectroscopic Confirmations of z ~ 7.0 Lya Emitting Galaxies in the LAGER Survey
窄带成像是发现大量z~6.6的高红移Lya发射星系（LAEs）的一种非常成功的方法。然而，在z> 7时，只有3个窄带选择性LAEs（2个在z~6.9-7.0，1个在z~7.3）得到了光谱证实，这阻碍了对这一关键时期宇宙再电离和星系演化的广泛研究。利用大面积窄带巡天LAGER（Lyman-Alpha Galerkin at the End of Reionization），我们在COSMOS场中选取了23个z~6.9的候选LAEs。在这项工作中，我们提出了12个候选人使用IMACS麦哲伦光谱的后续观测。对于其中的9个，观测足够深，可以检测到预期的线。在六个光源中识别出Lya发射线（成功率为2/3），包括3个发光的LAE，Lya光度为L（Lya）~ 10^{43.5} erg/s，是已知光谱证实的星系中最高的，>~7.0。这使光谱学确认的z>~7处的窄带选择LAE的样本大小增加了两倍，并确认了我们先前基于光度测量样本导出的Lya光度函数中的亮端凸起，支持斑片状再电离场景。两个发光的LAE出现物理联系，投影距离为1.1 pMpc，速度差为~ 170 km/s。它们可能位于由它们自己或与近邻产生的共同电离气泡中，这减少了Lya的IGM衰减。在一个源中可以看到一条暂时狭窄的NV $λ$ 1240线，暗示着中心大质量黑洞的活动，富含金属的线发射气体。
Massive Galaxies Form Early and Gray: Stellar Assembly and Dust Attenuation at $\mathbf{z>3.5}$ from CAPERS
The University of Texas at Austin（德克萨斯大学奥斯汀分校）；Cosmic Frontier Center, The University of Texas at Austin（德克萨斯大学奥斯汀分校宇宙前沿中心）；NSF’s National Optical-Infrared Astronomy Research Laboratory（美国国家光学-红外天文研究实验室）；Space Telescope Science Institute（太空望远镜科学研究所）
The Great Escape of ionizing photons during Cosmic Morning
Inter-University Centre for Astronomy and Astrophysics（国际天文学与天体物理中心）；Univ Lyon, Univ Lyon1, Ens de Lyon, CNRS, Centre de Recherche Astrophysique de Lyon UMR5574（里昂大学、里昂第一大学、巴黎高等师范学院里昂分校、法国国家科学研究中心、里昂天体物理研究中心）；Observatoire de Genève（日内瓦天文台）；Department of Physics & Waseda Research Institute for Science and Engineering, Faculty of Science and Engineering, Waseda University（早稻田大学理工学部物理系及理工学研究科）；Centre for Astrophysics Research, Department of Physics, Astronomy and Mathematics, University of Hertfordshire（赫特福德大学物理、天文与数学系天体物理研究中心）；Space Telescope Science Institute（太空望远镜科学研究所）；Department of Physics and Astronomy, Johns Hopkins University（约翰斯·霍普金斯大学物理与天文系）；School of Earth and Space Exploration, Arizona State University（亚利桑那州立大学地球与空间探索学院）；Minnesota State University-Mankato（明尼苏达州立大学曼卡托分校）
Spatially resolved H$α$ emission in B14-65666: compact starbursts, ionizing efficiency and gas kinematics in an advanced merger at the Epoch of Reionization
The Nature of High ${\rm [OIII]}_{\rm 88μm}$/${\rm [CII]}_{\rm 158μm}$ Galaxies in the Epoch of Reionization: Low Carbon Abundance and a Top-Heavy IMF?
Low Ly$α$ Visibility in Galaxy Overdensities: Reionization Topology and Neutral-Fraction Ceilings from DIVER over $4.8<z<11$
Steward Observatory, University of Arizona（亚利桑那大学斯图尔德天文台）；Institute for Astronomy, University of Edinburgh（爱丁堡大学天体物理研究所）；Department of Physics & Astronomy, University of California, Riverside（加州大学河滨分校物理与天文学系）；Department of Astronomy, Tsinghua University（清华大学天文系）；Department of Astronomy, Westlake University（西湖大学天文系）；School of Earth and Space Exploration, Arizona State University（亚利桑那州立大学地球与太空探索学院）；Department of Physics, University of Oxford（牛津大学物理系）
Highly-ionized gas in lensed z = 6.027 Little Red Dot seen through [OIII] 88$μ$m with ALMA
Chalmers University of Technology（查尔姆斯理工大学）；Durham University（杜伦大学）；University of KwaZulu-Natal（夸祖鲁-纳塔尔大学）；Universidade Federal do Rio de Janeiro（里约热内卢联邦大学）；University of Arizona（亚利桑那大学）；Columbia University（哥伦比亚大学）；Flatiron Institute（平顿研究所）
The JWST EXCELS Survey: A spectroscopic investigation of the ionizing properties of star-forming galaxies at 1<z<8
Institute for Astronomy, University of Edinburgh（爱丁堡大学天文研究所）；NSF’s National Optical-Infrared Astronomy Research Laboratory（美国国家光学-红外天文研究实验室）；Department of Astronomy, University of Massachusetts, Amherst（马萨诸塞大学阿默斯特分校天文学系）；Department of Physics & Astronomy, University of California（加州大学物理与天文学系）
REBELS-IFU: Steeply rising star formation histories and the importance of dust obscuration in massive $z \simeq7$ galaxies revealed by multi-wavelength observations
