银河系中心G+0.633-0.0604分子云：一个新的天体化学金矿：II. 化学丰富度
The Galactic centre G+0.633-0.0604 molecular cloud: A new astrochemical gold mine: II. Chemical richness
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- Centro de Astrobiología (CAB), CSIC-INTA（天体生物学中心）
- Universidad Complutense de Madrid（马德里康普顿斯大学）
- Max-Planck-Institut für extraterrestrische Physik（马克斯·普朗克地外物理研究所）
- European Southern Observatory（欧洲南方天文台）
- Joint ALMA Observatory（ALMA联合天文台）
- RIKEN（理化学研究所）
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中文总结 AI 辅助
该研究将银河系中心分子云G+0.633-0.0604确立为新的天体化学金矿，通过多望远镜巡天探测到15种复杂分子，证明其与G+0.693构成理想基准对，且线宽更窄，利于搜寻更复杂星际分子。
中文摘要 AI 辅助
近年来，星际分子的清单迅速增长，然而复杂物种的探测仅限于少数化学丰富的源，这引发了这样的疑问：这种复杂性究竟是真正罕见，还是由观测偏差所塑造。我们提出位于人马座B2复合体南部的银河系中心G+0.633-0.0604分子云，作为发现新星际分子的一个新的且极具前景的实验室。我们分析了G+0.633的高灵敏度分子谱线巡天数据，该巡天覆盖31$-$275 GHz频率范围内近100 GHz的聚合带宽，使用了Yebes 40米、IRAM 30米和APEX射电望远镜。G+0.633展现出极其丰富的分子原料，可与位于人马座B2北部的化学丰富云G+0.693相媲美，从而确立其作为G+0.693的“天体化学孪生体”的地位。我们报告了15种天体化学相关物种的新的可靠星际探测，其中大多数具有前生物意义，此前仅在G+0.693或极少数源中被识别。这些物种包括尿素、$C$-和$N$-氰甲亚胺、乙醇胺、乙醇酰胺、碳酸和二甲硫醚。我们的结果表明，在G+0.693中观测到的非凡分子复杂性并非独一无二，而可能反映了银河系中心激波主导化学的自然结果。G+0.633和G+0.693云展现出非常相似的激发条件和相当的分子丰度，确立了它们作为天体化学研究理想基准对的地位。此外，G+0.633在分子观测方面相比G+0.693具有明显优势，因为其分子谱线发射的线宽显著更窄，几乎只有G+0.693典型线宽的一半，使其成为指导搜寻星际介质中日益复杂分子的异常强大目标。
英文摘要
In recent years, the inventory of interstellar molecules has rapidly grown, yet detections of complex species are confined to a few chemically rich sources, raising the question of whether such complexity is genuinely rare or shaped by observational biases. We present the Galactic Centre G+0.633-0.0604 molecular cloud, located in the southern part of the Sgr B2 complex, as a new and very promising laboratory for the discovery of new interstellar molecules. We analysed data from a high-sensitivity molecular line survey of G+0.633, covering nearly 100 GHz of aggregated bandwidth over the 31$-$275 GHz frequency range with the Yebes 40m, IRAM 30m and APEX radio telescopes. G+0.633 exhibits an exceptionally rich molecular feedstock comparable to that of the chemically rich G+0.693 cloud in the northern part of Sgr B2, establishing it as its 'astrochemical twin'. We report new robust interstellar detections of 15 astrochemically relevant species, most of prebiotic interest, previously identified only in G+0.693 or a very limited number of sources. These species include urea, $C$- and $N$-cyanomethanimine, ethanolamine, glycolamide, carbonic acid, and dimethyl sulphide. Our results reveal that the extraordinary molecular complexity observed in G+0.693 is not unique, but may instead reflect a natural outcome of shock-dominated chemistry in the Galactic Centre. The G+0.633 and G+0.693 clouds exhibit remarkably similar excitation conditions and comparable molecular abundances, establishing them as an ideal benchmarking pair for astrochemical studies. Moreover, G+0.633 offers a clear advantage for molecular observations over G+0.693 owing to the significantly narrower linewidths of its molecular line emission, nearly half as broad as those characteristic of G+0.693, making it an exceptionally powerful target for guiding the search for increasingly complex molecules in the ISM.
