arXivDaily arXiv每日学术速递 周一至周五更新
arXiv 2207.04877astro-ph.GA
收藏

探测星际氰胺（NH $_{2}$ CN）朝向热分子核G10. 47 +0.03

Detection of interstellar cyanamide (NH$_{2}$CN) towards the hot molecular core G10.47+0.03

Arijit Manna, Sabyasachi Pal

备注：
10 pages, 4 figures
发表信息：
Journal of Astrophysics and Astronomy, 43, 83 (2022)
阅读 PDF
arXiv 页面 ↗HTML 原文 ↗

摘要：

在星际介质中，酰胺型分子在热分子核或高质量恒星形成区的生命起源分子的形成中起着重要的作用。氨腈（NH $_{2}$ CN）是一种在尿素（NH $_{2}$ CONH $_{2}$）形成中起主要作用的稀有星际分子。利用阿塔卡玛大型毫米/亚毫米波阵列（ALMA）干涉射电望远镜，在158.49 - 160.11 GHz频率范围内探测到了氨基氰（NH $_{2}$ CN）朝向热分子核G10.47+0.03的发射线。用旋转图模型估算了$_{2}$ CN的发射线的柱密度为：$N$（$_{2}$ CN）=（6.60 $\pm$ 0.1）$\times$ 10 $^{15}$ cm $^{-2}$，旋转温度（$T_{rot}$）= 201.2 $\pm$ 3.3 K. NH $_{2}$ CN相对于H $_{2}$向G10.47+0.03的丰度分数为$f$（NH $_{2}$ CN）= 5.076 $\times$ 10 $^{-8}$。此外，我们估计G10.47+0.03的NH $_{2}$ CN/NH $_{2}$ CHO丰度比为0.170，这与IRAS 16293 $-$ 2422 B和Sgr B2（M）的NH $_{2}$ CN/NH $_{2}$ CHO丰度比几乎相似。我们发现，观察到的NH $_{2}$ CN相对于H $_{2}$的丰度接近G10.47+0.03，与Garrod（2013）预测的理论值相当一致。我们还讨论了NH $_{2}$ CN可能的形成和破坏途径。

英文摘要：

In the interstellar medium, the amide-type molecules play an important role in the formation of the prebiotic molecules in the hot molecular cores or high-mass star formation regions. The complex amide-related molecule cyanamide (NH$_{2}$CN) is known as one of the rare interstellar molecule which has played a major role in the formation of urea (NH$_{2}$CONH$_{2}$). In this article, we presented the detection of the emission lines of cyanamide (NH$_{2}$CN) towards the hot molecular core G10.47+0.03 between the frequency range 158.49$-$160.11 GHz using the Atacama Large Millimeter/submillimeter Array (ALMA) interferometric radio telescope. The estimated column density of the emission lines of NH$_{2}$CN using the rotational diagram model was $N$(NH$_{2}$CN) = (6.60$\pm$0.1)$\times$10$^{15}$ cm$^{-2}$ with rotational temperature ($T_{rot}$) = 201.2$\pm$3.3 K. The fractional abundance of NH$_{2}$CN with respect to H$_{2}$ towards G10.47+0.03 was $f$(NH$_{2}$CN) = 5.076$\times$10$^{-8}$. Additionally, we estimated the NH$_{2}$CN/NH$_{2}$CHO abundance ratio towards the G10.47+0.03 was 0.170, which was nearly similar with NH$_{2}$CN/NH$_{2}$CHO abundance ratio towards IRAS 16293$-$2422 B and Sgr B2 (M). We found that the observed abundance of NH$_{2}$CN with respect to H$_{2}$ towards G10.47+0.03 fairly agrees with the theoretical value predicted by Garrod (2013). We also discussed the possible formation and destruction pathways of NH$_{2}$CN.

机构、总结、中文摘要均由AI分析而来，可能存在错误，请以论文正文为准。

↑