本文提出利用大质量黑洞导致的 Pop III 恒星潮汐瓦解事件进行探测，建模其 z~10 时的辐射与发生率，表明 JWST 和 Roman 可在红外波段发现此类暂现源，Roman 每年或可探测数十例。
摘要：
第一代无金属恒星被称为第三星族（Pop III）恒星，据信是在极早期宇宙中由原始气体形成的第一批天体。Pop III 恒星具有与当代恒星不同的结构，并且对于产生重元素和塑造后续恒星形成非常重要。然而，鉴于其高红移和短暂寿命，直接探测 Pop III 恒星极具挑战性。在本文中，我们提出了一种通过大质量黑洞引发的潮汐瓦解事件（TDE）来探测 Pop III 恒星的新方法。我们对这些独特 TDE 的辐射性质进行建模，并计算了它们在 z ~ 10 的早期宇宙中的预期发生率。我们发现，与本宇宙中太阳型恒星的 TDE 相比，Pop III 恒星 TDE 具有高得多的质量回落率和更长的演化时间尺度，这提高了其可探测性，尽管仍需要良好的巡天策略才能将这些源归类为暂现源。我们进一步证明，很大一部分耀发辐射会红移至红外波段，从而可由 James Webb Space Telescope 和 Nancy Grace Roman Space Telescope 探测。最后同样重要的是，基于我们目前对早期宇宙黑洞质量函数的理解，我们发现使用 Nancy Grace Roman Space Telescope 有望实现每年多达数十次的 Pop III 恒星 TDE 探测率。
英文摘要：
The first generation metal-free stars, referred to as population III (Pop III) stars, are believed to be the first objects to form out of the pristine gas in the very early Universe. Pop III stars have different structures from current generation of stars and are important for generating heavy elements and shaping subsequent star formation. However, it is very challenging to directly detect Pop III stars given their high redshifts and short life-times. In this paper, we propose a novel method for detecting Pop III stars through their tidal disruption events (TDEs) by massive black holes. We model the emission properties and calculate the expected rates for these unique TDEs in the early Universe at z ~ 10. We find that Pop III star TDEs have much higher mass fallback rates and longer evolution timescales compared to solar-type star TDEs in the local universe, which enhances the feasibility of their detection, although a good survey strategy will be needed for categorizing these sources as transients. We further demonstrate that a large fraction of the flare emissions are redshifted to infrared wavelengths, which can be detected by the James Webb Space Telescope and the Nancy Grace Roman Space Telescope. Last but not least, we find a promising Pop III star TDE detection rate of up to a few tens per year using the Nancy Grace Roman Space Telescope, based on our current understanding of the black hole mass function in the early Universe.
Tidal disruption event rates across cosmic time: forecasts for LSST, Roman, and JWST and their constraints on the supermassive black hole mass function
Johns Hopkins University（约翰斯·霍普金斯大学）；University of Maryland, College Park（马里兰大学帕克分校）
Signatures of Exploding Supermassive PopIII Stars at High Redshift in JWST, EUCLID and Roman Space Telescope
Max Planck Institute for Gravitational Physics (Albert Einstein Institute)（马克斯·普朗克引力物理研究所（爱因斯坦研究所））；Institute for Cosmic Ray Research, The University of Tokyo（东京大学宇宙射线研究所）；Center for Gravitational Physics and Quantum Information, Yukawa Institute for Theoretical Physics, Kyoto University（京都大学汤川理论物理中心引力物理与量子信息研究中心）；Frontier Research Institute for Interdisciplinary Sciences, Tohoku University（东北大学前沿交叉科学研究所）；Astronomical Institute, Graduate School of Science, Tohoku University（东北大学理学研究科天文学系）
Surveying the Universe in 4D: Beating Cosmic Variance with Wide-Field Slitless Spectroscopy from HST, JWST, Euclid, Roman, and Beyond
Space Telescope Science Institute（太空望远镜科学研究所）；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）；Beus Center for Cosmic Foundations, Arizona State University（亚利桑那州立大学宇宙基础布斯中心）；NASA/GSFC（美国国家航空航天局戈达德太空飞行中心）；Massachusetts Institute of Technology（麻省理工学院）
Numerical Simulations of the Circularized Accretion Flow in Population III Star Tidal Disruption Events. II. Radiative Properties
Shanghai Astronomical Observatory, Chinese Academy of Sciences（中国科学院上海天文台）；University of Chinese Academy of Sciences（中国科学院大学）；Shanghai Normal University（上海师范大学）；State Key Laboratory of Particle Astrophysics, Institute of High Energy Physics, Chinese Academy of Sciences（中国科学院高能物理研究所粒子天体物理国家重点实验室）；Chongqing University（重庆大学）
JWST and Keck observations of the off-nuclear tidal disruption event TDE 2025abcr: An evolving reprocessing layer
UC Santa Cruz（加州大学圣克鲁兹分校）；University of California Observatories（加州大学天文台）；University of California, Berkeley（加州大学伯克利分校）；University of Illinois at Urbana-Champaign（伊利诺伊大学厄巴纳-香槟分校）；Center for Astrophysics | Harvard & Smithsonian（哈佛史密森尼天体物理中心）；University of Texas Austin（德克萨斯大学奥斯汀分校）
A tidal disruption event in a quasar at redshift 7.19
University of Toronto（多伦多大学）；Dunlap Institute for Astronomy and Astrophysics, University of Toronto（多伦多大学邓普天文学与天体物理研究所）；Cosmic Dawn Center (DAWN)（宇宙黎明中心）；Niels Bohr Institute, University of Copenhagen（哥本哈根大学尼尔斯·玻尔研究所）；Kavli Institute for Astronomy and Astrophysics, Peking University（北京大学科维理天文与天体物理研究所）；Department of Astronomy, School of Physics, Peking University（北京大学物理学院天文学系）；The University of Texas at Austin（德克萨斯大学奥斯汀分校）；Max-Planck-Institut für extraterrestrische Physik（马克斯·普朗克地外物理学研究所）
SN 2025ogs: A Spectroscopically-Normal Type Ia Supernova at z = 2 as a Benchmark for Redshift Evolution
Space Telescope Science Institute（太空望远镜科学研究所）；Johns Hopkins University（约翰斯·霍普金斯大学）；University of Arizona（亚利桑那大学）；Oklahoma State University（俄克拉荷马州立大学）；University of California, Santa Cruz（加利福尼亚大学圣克鲁兹分校）
SN 2025ogs在z=2.05的红移下表现出正常Ia型超新星特性，其光谱和光变曲线符合标准模型，为未来高红移Ia型超新星样本提供基准，验证了Ia型超新星标准化在高红移下的稳定性。
ACORN I. Massive Black Hole Seeding and Tidal Disruption Events from Star Clusters in Cosmological Simulations
Carnegie Mellon University（卡内基梅隆大学）；UCLA（加州大学洛杉矶分校）；University of Virginia（弗吉尼亚大学）；Universidade de Santiago de Compostela（圣地亚哥德孔波斯特拉大学）；University of North Carolina at Chapel Hill（北卡罗来纳大学教堂山分校）；Northwestern University（西北大学）；University of Florida（佛罗里达大学）
Hubble as a Unique Discovery Engine of the Fate of Massive Stars and Black Hole Formation
Institute of Astronomy, University of Cambridge（剑桥大学天文学研究所）；Institute of Astronomy, KU Leuven（荷语鲁汶大学天文学研究所）；Leuven Gravity Institute, KU Leuven（荷语鲁汶大学引力研究所）；Anton Pannekoek Institute for Astronomy, University of Amsterdam（阿姆斯特丹大学安东·潘内科克天文学研究所）；Center for Interdisciplinary Exploration and Research in Astrophysics (CIERA), Northwestern University（西北大学天体物理学跨学科探索与研究中心）；David A. Dunlap Department of Astronomy and Astrophysics, University of Toronto（多伦多大学戴维·A·邓普天文学与天体物理学系）；Observatories of the Carnegie Institution for Science（卡内基科学机构天文台）；McWilliams Center for Cosmology and Astrophysics, Department of Physics, Carnegie Mellon University（卡内基梅隆大学物理学院麦克威廉斯宇宙学与天体物理学中心）
California Institute of Technology（加州理工学院）；Massachusetts Institute of Technology（麻省理工学院）；Center for Astrophysics, Harvard and Smithsonian（哈佛史密松天体物理中心）；Max-Planck-Institut für Astronomie（马克斯·普朗克天文研究所）；Institute for Astronomy, University of Hawaii（夏威夷大学天体物理研究所）
