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Neutral Hydrogen 21-cm Signature Originated from the First Generation of Stars in the Universe

田中, 俊行 名古屋大学

2021.06.21

概要

宇宙の第一世代の恒星は初代星と呼ばれ、宇宙の熱史や構造形成史において重要な役割を担う。その重要性を決定づける星質量などの物理的性質は主に理論研究によって調べられてきたが、各研究間で未だ合意形成に至っていない。一方、観測においては、中性水素の超微細構造に由来する波長21cmの光（21-cm線）を捉える大規模電波望遠鏡であるSquare Kilometre Array(SKA)が建設中であり、2020年代後半には初代星に由来するシグナルの初検出が期待されている。しかし、将来観測との比較に耐えうる精度を持つ理論モデルは存在せず、その構築は喫緊の課題である。

申請者はまず、個々の初代星が周囲の中性水素からの21-cm線シグナルに及ぼす影響を明らかにするための理論的研究を実施した。これまでに考慮されてこなかった流体力学的な時間変化を取り入れた輻射流体シミュレーションコードを開発し、初代星の形成場所であるハロー内部の高密度ガスを含む、周囲のガスの状態を計算した。その結果、高密度ガスの流体力学的効果により、21-cm線シグナル構造の時間進化に2つの段階があることを発見した。第一段階では、初代星周囲の電離領域が高密度ガスによって閉じ込められ、その電離領域の外側に21-cm線の深い吸収線領域が形成される。その後、高密度ガスが熱膨張することで密度が下がり、電離領域が高密度ガス領域を超えて拡大する。この第二段階において、21-cm線シグナル構造はこれまで知られていた構造に漸近する。また申請者は、第一段階で形成される深い吸収線領域はシグナル強度が強く、従来考えられていたより観測的に検出されやすいことを示した。さらに、恒星周囲のシグナル構造の星質量、ハロー質量、赤方偏移依存性を明らかにした。得られた21-cm線シグナル構造をさらに解析することで、(1)SKAを用いても個々の初代星からのシグナルの観測は困難であること、(2)比較的観測しやすい21-cm線シグナルの全天平均値（グローバルシグナル）は星質量の情報を反映すること、(3)グローバルシグナルにおいて星質量と星形成率密度が縮退することの3点を明らかにした。

次に申請者は、宇宙論的スケールにおける初代星起源21-cm線シグナルに関する理論的研究を実施した。宇宙論的シミュレーションのサブグリッドスケールに対応する物理過程、具体的には(ア)電離光子脱出率のハロー質量と星質量依存性、(イ)初代星からの紫外線によるガス加熱、について、上記の輻射流体シミュレーションの結果を取り入れることで考慮できる手法を開発した。その手法を公開されている準数値的シミュレーションコードである21cmFASTに組み込み、各物理過程が21-cm線観測量へ与える影響を調査した。申請者はシミュレーションデータを解析することで、星から放射が水素分子を解離にすることにより星形成可能な最小ハロー質量が時間と共に増加し、電離光子脱出率の平均値が小さくなることを明らかにした。その結果、ハローから脱出し銀河間物質の電離に寄与する電離光子が減少し、宇宙の電離度が低く推移することが示された。また、宇宙の平均電離度が約１％を超える時代には、紫外線によるガス加熱の影響が無視できないことがわかった。さらに、申請者はグローバルシグナルに加え、21-cm線シグナルの空間非一様性の情報を用いることで、星質量と星形成率密度の縮退が解けることを示した。

本研究を通して申請者は、個々の初代星周囲のシグナルが流体力学的効果により、従来予測されていたより強いシグナルとなることを示したが、それでもなお、電波望遠鏡による個別の初代星の観測は困難である。一方、宇宙論的スケールのシグナルにおいては、初代星が宇宙の電離に寄与する場合、21-cm線観測量から初代星の物理的性質を推定できる可能性があることを示した。

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