The nature of an ultra-faint galaxy in the cosmic dark ages seen with JWST,Nature

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The nature of an ultra-faint galaxy in the cosmic dark ages seen with JWST
Nature ( IF 50.5 ) Pub Date : 2023-05-17 , DOI: 10.1038/s41586-023-05994-w
Guido Roberts-Borsani ₁ , Tommaso Treu ₁ , Wenlei Chen ₂ , Takahiro Morishita ₃ , Eros Vanzella ₄ , Adi Zitrin ₅ , Pietro Bergamini _{4,

6} , Marco Castellano ₇ , Adriano Fontana ₇ , Karl Glazebrook ₈ , Claudio Grillo _{6,

9} , Patrick L Kelly ₂ , Emiliano Merlin ₇ , Themiya Nanayakkara ₈ , Diego Paris ₇ , Piero Rosati _{4,

10} , Lilan Yang ₁₁ , Ana Acebron _{6,

9} , Andrea Bonchi _{7,

12} , Kit Boyett _{13,

14} , Maruša Bradač _{15,

16} , Gabriel Brammer _{17,

18} , Tom Broadhurst _{19,

20,

21} , Antonello Calabró ₇ , Jose M Diego ₂₂ , Alan Dressler ₂₃ , Lukas J Furtak ₅ , Alexei V Filippenko ₂₄ , Alaina Henry _{25,

26} , Anton M Koekemoer ₂₅ , Nicha Leethochawalit ₂₇ , Matthew A Malkan ₁ , Charlotte Mason _{17,

18} , Amata Mercurio _{28,

29} , Benjamin Metha _{1,

13,

14} , Laura Pentericci ₇ , Justin Pierel ₂₅ , Steven Rieck ₂ , Namrata Roy ₂₆ , Paola Santini ₇ , Victoria Strait _{17,

18} , Robert Strausbaugh ₃₀ , Michele Trenti _{13,

14} , Benedetta Vulcani ₃₁ , Lifan Wang ₃₂ , Xin Wang _{33,

34,

35} , Rogier A Windhorst ₃₆

Affiliation

Department of Physics and Astronomy, University of California, Los Angeles, CA, USA.
School of Physics and Astronomy, University of Minnesota, Minneapolis, MN, USA.
Infrared Processing and Analysis Center, Caltech, Pasadena, CA, USA.
INAF - OAS, Osservatorio di Astrofisica e Scienza dello Spazio di Bologna, Bologna, Italy.
Physics Department, Ben-Gurion University of the Negev, Be'er-Sheva, Israel.
Dipartimento di Fisica, Università degli Studi di Milano, Milan, Italy.
INAF Osservatorio Astronomico di Roma, Monteporzio Catone, Rome, Italy.
Centre for Astrophysics and Supercomputing, Swinburne University of Technology, Hawthorn, Victoria, Australia.
INAF - IASF Milano, Milan, Italy.
Dipartimento di Fisica e Scienze della Terra, Università degli Studi di Ferrara, Ferrara, Italy.
Kavli Institute for the Physics and Mathematics of the Universe, The University of Tokyo, Kashiwa, Japan.
ASI-Space Science Data Center, Rome, Italy.
School of Physics, University of Melbourne, Parkville, Victoria, Australia.
ARC Centre of Excellence for All Sky Astrophysics in 3 Dimensions (ASTRO 3D), Canberra, Australian Capital Territory, Australia.
University of Ljubljana, Department of Mathematics and Physics, Ljubljana, Slovenia.
Department of Physics and Astronomy, University of California, Davis, CA, USA.
Cosmic Dawn Center (DAWN), Copenhagen, Denmark.
Niels Bohr Institute, University of Copenhagen, Copenhagen, Denmark.
Department of Theoretical Physics, University of the Basque Country UPV/EHU, Bilbao, Spain.
Donostia International Physics Center (DIPC), Donostia, Spain.
IKERBASQUE, Basque Foundation for Science, Bilbao, Spain.
Instituto de Física de Cantabria (CSIC-UC), Santander, Spain.
The Observatories, The Carnegie Institution for Science, Pasadena, CA, USA.
Department of Astronomy, University of California, Berkeley, CA, USA.
Space Telescope Science Institute, Baltimore, MD, USA.
Center for Astrophysical Sciences, Department of Physics & Astronomy, Johns Hopkins University, Baltimore, MD, USA.
National Astronomical Research Institute of Thailand (NARIT), Mae Rim, Thailand.
Dipartimento di Fisica 'E.R. Caianiello', Università degli Studi di Salerno, Fisciano (SA), Italy.
INAF-Osservatorio Astronomico di Capodimonte, Naples, Italy.
Minnesota Institute For Astrophysics, University of Minnesota, Minneapolis, MN, USA.
INAF Osservatorio Astronomico di Padova, Padova, Italy.
Mitchell Institute for Fundamental Physics & Astronomy, Texas A&M University, Department of Physics and Astronomy, College Station, TX, USA.
School of Astronomy and Space Science, University of Chinese Academy of Sciences (UCAS), Beijing, China.
National Astronomical Observatories, Chinese Academy of Sciences, Beijing, China.
Institute for Frontiers in Astronomy and Astrophysics, Beijing Normal University, Beijing, China.
School of Earth and Space Exploration, Arizona State University, Tempe, AZ, USA.

In the first billion years after the Big Bang, sources of ultraviolet (UV) photons are believed to have ionized intergalactic hydrogen, rendering the Universe transparent to UV radiation. Galaxies brighter than the characteristic luminosity L* (refs. ^1,2) do not provide enough ionizing photons to drive this cosmic reionization. Fainter galaxies are thought to dominate the photon budget; however, they are surrounded by neutral gas that prevents the escape of the Lyman-α photons, which has been the dominant way to identify them so far. JD1 was previously identified as a triply-imaged galaxy with a magnification factor of 13 provided by the foreground cluster Abell 2744 (ref. ³), and a photometric redshift of z ≈ 10. Here we report the spectroscopic confirmation of this very low luminosity (≈0.05 L*) galaxy at z = 9.79, observed 480 Myr after the Big Bang, by means of the identification of the Lyman break and redward continuum, as well as multiple ≳4σ emission lines, with the Near-InfraRed Spectrograph (NIRSpec) and Near-InfraRed Camera (NIRCam) instruments. The combination of the James Webb Space Telescope (JWST) and gravitational lensing shows that this ultra-faint galaxy (M_UV = −17.35)—with a luminosity typical of the sources responsible for cosmic reionization—has a compact (≈150 pc) and complex morphology, low stellar mass (10^7.19 M_⊙) and subsolar (≈0.6 Z_⊙) gas-phase metallicity.

中文翻译：

JWST 观测到的宇宙黑暗时代超微弱星系的性质

在大爆炸后的第一个十亿年里，紫外线 (UV) 光子的来源被认为已经电离了星际氢，使宇宙对紫外线辐射透明。比特征光度L *（参考文献 ^1,2）亮的星系不能提供足够的电离光子来驱动这种宇宙再电离。较暗的星系被认为支配着光子预算；然而，它们被中性气体包围，阻止了莱曼-α光子的逃逸，而莱曼-α光子一直是迄今为止识别它们的主要方式。^{JD1 之前被确定为一个三重成像星系，其放大倍数为 13，由前景星团 Abell 2744（参考文献3} ）提供，光度红移为z ≈ 10。在这里，我们报告了在大爆炸后 480 Myr 观察到的这个极低光度 (≈0.05 L *) 星系在z = 9.79 处的光谱确认，方法是识别莱曼断裂和红向连续体，以及多条≳ 4 σ发射线，使用近红外光谱仪 (NIRSpec) 和近红外相机 (NIRCam) 仪器。詹姆斯·韦伯太空望远镜 (JWST) 和引力透镜的结合表明，这个超微弱星系 ( M _UV = −17.35)——具有负责宇宙再电离源的典型光度——具有紧凑的 (≈150 pc) 和复杂_的形态，低恒星质量（10 ^7.19 M⊙) 和次太阳 (≈0.6 _Z⊙ )气相金属丰度。

更新日期：2023-05-18

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