星際分子列表

星際分子列表列出已在星際物質和星周包層中被檢測出的分子，並依照組成原子的數目分組。每一種分子均附其化學式，若有離子型式也會一併列出。 本列表中的所有分子都是透過分光學檢測出來的。這些分子的光譜特徵是由不同能級之間組成電子的躍遷，或是通過旋轉、振動光譜產生的，多數會在光譜的無線電波、微波或紅外線部分被偵測出來。 星際分子是由非常稀疏的星際或星周雲內的塵埃和氣體經化學反應而形成的，大部分時候於分子與宇宙射線相互作用、被電離時發生。射線中帶正電的質點會以靜電力吸引鄰近的中性粒子。反應也可以在中性的原子和分子之間發生，但進行的比較緩慢。塵埃在使分子免受恆星發出的紫外線輻射的電離效應上具有關鍵作用。 生命的化學反應可能開始於距今約138億年前的大霹靂不久之後、宇宙進入一段適居時期時，當時宇宙的年齡約只有1億至1.7億年。 在星際物質中檢測到的第一個含碳分子是甲炔（CH•），於1937年首次被檢測出來。之後的20世紀70年代早期的一些證據顯示，宇宙塵埃是由數量眾多的複雜有機分子（COMs，可能是聚合物）所組成的。天體物理學家錢德拉·維克拉瑪辛赫（英语：Chandra Wickramasinghe）以甲醛分子為基礎提出聚合化合物存在於星際空間中的可能；維克拉瑪辛赫並與弗雷德·霍伊爾據2175 Å的紫外線消光吸收分析鑑定出了雙環芳香族化合物的存在，從而證明了星際空間中存在著多環芳香烴分子。 2004年，科學家在自紅矩形星雲發射的紫外線中檢測出了蒽和芘的光譜特徵（英语：Spectral signature），此等複雜的分子之前從未在外太空中被發現。學界多認為此一發現證實了當與紅矩形星雲相同類型的星雲接近生命盡頭時，星雲核心中的碳和氫將因對流作用被束縛在恆星風中並向外輻射的假設：當冷卻時，原子會彼此結合，最終形成含有百萬顆以上原子的大型分子。科學家們並推斷，既然多環芳香烴是在星雲中被發現的，那其必然也是產生於星雲之中。 2010年，富勒烯（又稱為「巴克球」）在星雲中被檢測出來。富勒烯與生命起源有著一定的關係；天文學家萊蒂西亞·史坦赫利尼（Letizia Stanghellini）表示：「來自外太空的巴克球有可能為地球上的生命發展提供了種子。」2019年4月，科學家透過哈伯太空望遠鏡觀測星際物質時，在恆星間偵測到了大型、複雜的離子化巴克明斯特富勒烯（C60）分子。 2011年，科學家們利用光譜學發現，含有複雜有機化合物（「具有芳香族－脂肪族混合結構的無定形有機固體」）的宇宙塵埃可自然、快速地由恆星產生。這些分子的化學結構非常複雜，其複雜程度已可與煤和石油的化學成分相比；之前學界普遍認為具有這種複雜程度的化學物質僅能由生物體產生。觀察結果表明，由星際塵埃粒子引入地球的有機化合物基於其表面催化活性可以作為生命的基本要素。其中一位科學家並認為這些化合物可能與地球上的生命發展相關，並表示：「如果這一假設為真，則地球上的生命可能會比我們想像的更容易萌芽，因為這些有機物可以作為生命的組成基礎。」 2012年8月，哥本哈根大學的天文學家在一個遙遠星系中的原恆星周圍發現了乙醇醛（一種有機化合物）；此恆星的編號為IRAS 16293-2422，距離地球約400光年。乙醇醛是組成核糖核酸的必要物質之一，而核糖核酸可在遺傳編碼、轉譯、調控及基因表現等過程中發揮作用。這一發現表明複雜的有機分子可能在行星形成之前即在恆星系統中產生，並最終到達正在發展的早期行星上。 2012年9月，美國國家航空暨太空總署的科學家提出報告，認為多環芳香烴在星際物質環境中會經氫化、氧化及羥基化等作用形成更複雜的有機化合物，「逐步向形成核苷酸和胺基酸（分別為蛋白質和去氧核醣核酸）的道路前進」。此外，在轉變的過程中，多環芳香烴物質將喪失其光譜特徵，「或許就是為什麼在星際冰（英语：Interstellar ice）（尤其是寒冷、濃密的星雲）及原行星盤的上部分子層中很少偵測到多環芳香烴存在的原因之一」。 多環芳香烴在宇宙中隨處可見。2013年6月，多環芳香烴在土星最大的衛星土衛六（俗稱「泰坦」）上被偵測出來。 2013年8月，里兹大學的德威恩·赫德（Dwayne Heard）認為量子力學中的量子穿隧效應可以解釋他的實驗小組觀察到的現象：冷羥基（溫度約63克耳文）和甲醇分子之間突破了分子內的能壘，導致兩種物質之間的反應發生率明顯高於預期。在不考慮量子效應時，此分子能壘一般需在較高溫度的環境中透過熱能或電離作用克服。量子穿隧效應有助於解釋複雜分子（由數十個以上的原子所組成）於星際空間中的存在。 2015年3月，NASA的科學家報告其實驗室已成功利用嘧啶（常見於隕石中）等基本化學物質，在外太空模擬環境下生成包括尿嘧啶、胞嘧啶和胸腺嘧啶在內的DNA和RNA等複雜有機化合物。據科學家的說法，嘧啶的形成過程與多環芳香烴相似，可能是在紅巨星、星際塵埃或氣體雲中生成的。 2016年10月，天文學家稱甲炔、碳氫正離子（CH+）和碳離子（C+）等生命形成所需的基本要素大部分是自恆星發出的紫外線中產生的，而非像之前料想的與超新星和年輕恆星擾動相關的事件等其他生成途徑。 人馬座B2是宇宙中星際分子含量最豐富的區域之一。人馬座B2是一個由氣體和塵埃組成的分子雲，橫躺在銀河系的中心附近，常成為天文學的研究標的。本列表中大約有一半的分子最初都是在人馬座B2內被發現的，而幾乎所有已知的星際分子目前也都能在此處檢測出來。另一個常作為星際分子調查來源的地點是獅子座CW（即IRC +10216星），有多達50種分子在那裡被檢測出來。 要解釋觀察到的異構物的比例，就必須運用最小能量原理。在大多數情況中，最小能量原理能夠解釋為何某些分子因為總能量較低的緣故在星際空間的含量較其異構物豐富，不過也有一些例外存在。這些例外有些可以利用其他分子參數解決，例如偶極極化率（dipole polarizabilty）也會影響異構物的豐度：極化率較低的分子在星際空間的含量會比平均極化率較高的分子更豐富。此現象的成因來自於與宇宙中各種輻射原理相似之極化率與外部電場下分子行為的相關性。 另一種解釋則完全忽略能量問題，只處理透過資訊熵指數（information entropy index）計算的分子複雜性。此解釋推測一些分子的組成物質參數值（如尿素、嘧啶、二羥基丙酮、尿嘧啶、胞嘧啶、甘氨酸和丙氨酸等）因落入已知星際分子典型值的範圍內，使這些分子在星際環境中被發現的可能性較其他分子要高。此外，資訊熵大的分子，即那些結構最複雜的分子，占有星際集合的一半之多，其百分比隨著分子大小而遞減。此一趨勢也有可能與分子化學結構之均勻度和穩定性的不同有關，因為大尺寸的可檢測分子更可能擁有對稱而非不對稱的分子結構。實際觀察中檢測到的大量低熵、結構高度對稱的富勒烯分子為這一假設提供了支持理據。另外，資訊熵也反映了物質的氫化深度：資訊熵大的分子缺少氫氣組成，而其他多數分子皆含有大量的氫。 下列出已在星際物質和星周包層中被檢測出的分子，並依照組成原子的數目分組。每一種分子均附其化學式，若有離子型式也會一併列出。若該分子只有離子型式被檢測出來，或是沒有在科學文獻中定名者，則分子一欄留空。下列表格中質量一格數據採用之計量單位為原子質量單位。每小節標題會列出該小節所含之分子總數。 目前大部分被偵測出的星際分子都是有機化合物。在所有組成原子數目達五個以上的分子中，只有甲矽烷（SiH4）是無機化合物，其他分子都具有至少一個碳原子，而沒有N-N或O-O鍵。 以下分子皆含有氘（D/2 H），氫的一種穩定形態同位素。 以下分子存在於星際空間中的證據曾在科學文獻中被提及，然而這些證據不是被文獻作者描述為「暫定性的」，就是曾被其他學者所挑戰。這些分子存在於星際空間中的證據仍待更多獨立研究證實。 化学主题 物理学主题 天文学主题 生命起源 天體生物學 天文化學 原子和分子天體物理學（英语：Atomic and molecular astrophysics） 宇宙塵埃 宇宙射線 宇宙化學 瀰漫星際譜帶（英语：Diffuse interstellar band） 地外液態水 禁線 星系際塵埃 行星際物質 星際物質 分子列表（英语：Lists of molecules） 有機化合物列表 有機化學 非蛋白胺基酸 有機化合物 外太空 泛種論 多環芳香烴 芳香性 光譜學 托林 Shu, Frank H. 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