星間分子の一覧

このリストは、天体望遠鏡を用いて行われた分子雲、原始惑星系円盤等からの電磁波観測により発見され、同定された星間分子の一覧（せいかんぶんしのいちらん）である。リストは構成原子毎に挙げた。イオンが検出されている分子についてはそれも示した。 以下に示すのは恒星間の希薄空間（星間空間）に存在する分子（星間分子）のうち分光学的な手法により確認された分子の一覧である。 光学望遠鏡や電波望遠鏡を用いることで、天体から発せられる電磁波のスペクトルが得られる。ある分子の異なった電子状態、振動準位または回転準位間の遷移は、スペクトルの中でその分子に特徴的な波長や周波数に吸収や発光として観測される。これらのスペクトルは電波、マイクロ波および赤外線、可視光、紫外線の周波数領域で観測される。（詳しくは宇宙化学を参照）。これらの中で一番初めに同定された星間分子は1937年に観測され、1940年にCNなどとともに同定されたメチリジンラジカル (CH) である。 星間分子は非常に希薄な星間空間や、星周辺領域の分子雲の中で化学反応を通して形成される。この化学反応のうちの多くは分子が（特に陽イオンへ）イオン化されたときに起こる。イオン化はしばしば宇宙線との相互作用によって行われ、そのため、陽イオンは星間空間において数多く存在する。この陽イオンは周辺の電荷を持たない分子を静電気的な引力により引き込み反応を起こす。（詳細はイオン-分子反応へ）イオンと分子の反応よりは遅いが、電荷を持たない分子同士の反応によっても、星間分子は生成されている。 特に多量にそして他種類の分子が観測される天体として、サジタリウスB2分子雲 (Sagittarius B2; Sgr B2)が挙げられる。この巨大な分子雲は天の川銀河の中心方向にほど近く、新しい分子の検出を目的とする研究ではよく探索が行われる。以下のリストのおよそ半分の分子はこのSgr B2分子雲において初めに検出が行われており、そのほかの分子についても近い将来検出されるであろう。 以下の表では検出された星間分子を構成原子数ごとに分けてリストアップしている。分子の列に記入がないものはイオンだけが検出されていることを示す。名称の列に記入のないものはこれまでに科学文献で名称が与えられていない分子である。（和名は日本語において慣用的に用いられるものを示した。） なお、存在量としては水素分子が圧倒的に多く、次いでCO（一酸化炭素）、H2O（水）、NH3（アンモニア）、HCHO（ホルムアルデヒド）、HCN（シアン化水素）の順で多い。 以下の分子は科学文献において検出が報告されているが、その後他の科学者による確認がなされていない分子である。 [脚注の使い方] ^ a b Nummelin, Albert (2006年7月13日). “Observations of interstellar molecules”. 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Dyubko (2005). “A Rigorous Attempt to Verify Interstellar Glycine”. Astrophysical Journal 619 (2): 914-930. http://adsabs.harvard.edu/abs/2004astro.ph.10335S.  ^ S. L. Widicus Weaver, G. A. Blake (2005). “1,3-Dihydroxyacetone in Sagittarius B2(N-LMH): The First Interstellar Ketose”. Astrophysical Journal 624 (2): L33–L36. doi:10.1086/430407. https://iopscience.iop.org/article/10.1086/430407/pdf.  天文学 化学 星間物質 宇宙化学 岡山大学理学部化学科分光化学研究室 データー集の中に星間分子のリストを掲載 Interstellar and circumstellar molecules by David Woon List of interstellar molecules by Andrew Markwick-Kemper List of interstellar and circumstellar molecules from NASA's Cosmic Ice Lab NRAO Interstellar and Circumstellar Molecules by Al Wootten Observations of interstellar molecules by Albert Nummelin