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研究分野物理科学凝縮物質物理学凝縮物質の電子および磁気特性;超伝導性
研究分野
物理科学
凝縮物質物理学
凝縮物質の電子および磁気特性;超伝導性
ビッグバンから2億5千万年後の恒星形成の始まり

ビッグバンから2億5千万年後の恒星形成の始まり

Takuya Hashimoto ^1,2, Nicolas Laporte ^3,4, Ken Mawatari ⁵, Richard S Ellis ³, Akio K Inoue ⁵, Erik Zackrisson ⁶, Guido Roberts-Borsani ³, Wei Zheng ⁷, Yoichi Tamura ⁸, Franz E Bauer ^9,10,11, Thomas Fletcher ³, Yuichi Harikane ^12,13, Bunyo Hatsukade ¹⁴, Natsuki H Hayatsu ^13,15, Yuichi Matsuda ^16,17, Hiroshi Matsuo ^16,17, Takashi Okamoto ¹⁸, Masami Ouchi ^12,19, Roser Pelló ⁴, Claes-Erik Rydberg ²⁰, Ikkoh Shimizu ²¹, Yoshiaki Taniguchi ²², Hideki Umehata ^14,22,23, Naoki Yoshida ^13,19

Takuya Hashimoto ^1,2, Nicolas Laporte ^3,4, Ken Mawatari ⁵

¹Department of Environmental Science and Technology, Faculty of Design Technology, Osaka Sangyo University, Osaka, Japan. thashimoto@est.osaka-sandai.ac.jp.
²National Astronomical Observatory of Japan, Tokyo, Japan. thashimoto@est.osaka-sandai.ac.jp.
³Department of Physics and Astronomy, University College London, London, UK.
⁴IRAP, Université de Toulouse, CNRS, UPS, CNES, Toulouse, France.
⁵Department of Environmental Science and Technology, Faculty of Design Technology, Osaka Sangyo University, Osaka, Japan.
⁶Department of Physics and Astronomy, Uppsala University, Uppsala, Sweden.
⁷Department of Physics & Astronomy, Johns Hopkins University, Baltimore, MD, USA.
⁸Division of Particle and Astrophysical Science, Graduate School of Science, Nagoya University, Nagoya, Japan.
⁹Instituto de Astrofísica and Centro de Astroingeniería, Facultad de Física, Pontificia Universidad Católica de Chile, Santiago, Chile.
¹⁰Millennium Institute of Astrophysics (MAS), Santiago, Chile.
¹¹Space Science Institute, Boulder, CO, USA.
¹²Institute for Cosmic Ray Research, The University of Tokyo, Chiba, Japan.
¹³Department of Physics, Graduate School of Science, The University of Tokyo, Tokyo, Japan.
¹⁴Institute of Astronomy, The University of Tokyo, Tokyo, Japan.
¹⁵European Southern Observatory, Garching bei München, Germany.
¹⁶National Astronomical Observatory of Japan, Tokyo, Japan.
¹⁷Department of Astronomical Science, School of Physical Sciences, The Graduate University for Advanced Studies (SOKENDAI), Tokyo, Japan.
¹⁸Department of Cosmosciences, Graduates School of Science, Hokakido University, Sapporo, Japan.
¹⁹Kavli Institute for the Physics and Mathematics of the Universe (WPI), Todai Institutes for Advanced Study, The University of Tokyo, Chiba, Japan.
²⁰Universität Heidelberg, Zentrum für Astronomie, Institut für Theoretische Astrophysik, Heidelberg, Germany.
²¹Theoretical Astrophysics, Department of Earth and Space Science, Osaka University, Osaka, Japan.
²²The Open University of Japan, Chiba, Japan.
²³The Institute of Physical and Chemical Research (RIKEN), Saitama, Japan.

⁰Department of Environmental Science and Technology, Faculty of Design Technology, Osaka Sangyo University, Osaka, Japan. thashimoto@est.osaka-sandai.ac.jp.

Nature +

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2018年5月18日

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2018年5月18日

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PubMedで要約を見る

まとめ

この要約は機械生成です。

天文学者はビッグバンから2億5000万年後に形成された初期の銀河MACS1149-JD1を検出しましたこの発見により宇宙の初期と銀河の形成の理解が進んでいます

科学分野

宇宙の誕生と初期の宇宙の研究
銀河の形成と進化
銀河間媒体の濃縮

背景

最古の銀河の位置づけは現代天文学の重要な課題です
恒星形成の銀河の数は赤道偏移6から10に減少します
初期の銀河の星形成を理解することはまだ課題です

研究の目的

初期の宇宙時代の星形成の範囲を調査する
重力レンズ銀河MACS1149-JD1を観察し分析する
初期の恒星群の形成期を決定する.

主な方法

重力レンズ銀河MACS1149-JD1のスペクトル観測
二重イオン化された酸素排出ラインの検出
スペクトル特性を用いて赤偏移を正確に測定する.

主要な成果

赤色偏移 9.1096 ± 0.0006 で二重イオン化された酸素放射線を検出した.
銀河の赤い光学色は,ビッグバンから約2億5000万年後に形成された支配的な恒星集団を示しています (赤色移転約15).
宇宙が現在の年齢の4%以下だった時に観測された銀河の初期恒星形成が確認された.

結論

MACS1149-JD1は最初の銀河の星形成の証拠を提供します
初期の恒星形成のエピソードは類似の銀河で検出できます
未来の望遠鏡は初期の恒星形成を検出するかもしれません

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