تقرير
ATOMS: ALMA Three-millimeter Observations of Massive Star-forming regions -- X. Chemical differentiation among the massive cores in G9.62+0.19
| العنوان: | ATOMS: ALMA Three-millimeter Observations of Massive Star-forming regions -- X. Chemical differentiation among the massive cores in G9.62+0.19 |
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| المؤلفون: | Peng, Y. P., Liu, T., Qin, S. -L., Baug, T., Liu, H. -L., Wang, K., Garay, G., Zhang, C., Chen, L. -F., Lee, C. W., Juvela, M., Li, D. L., Tatematsu, K., Liu, X. -C., Lee, J. -E., Luo, G., Dewangan, L., Wu, Y. -F., Zhang, L., Bronfman, L., Ge, J. X., Tang, M. Y., Zhang, Y., Xu, F. -W., Wang, Y., Zhou, B. |
| سنة النشر: | 2022 |
| المجموعة: | Astrophysics |
| مصطلحات موضوعية: | Astrophysics - Astrophysics of Galaxies |
| الوصف: | Investigating the physical and chemical structures of massive star-forming regions is critical for understanding the formation and the early evolution of massive stars. We performed a detailed line survey toward six dense cores named as MM1, MM4, MM6, MM7, MM8, and MM11 in G9.62+0.19 star-forming region resolved in ALMA band 3 observations. Toward these cores, about 172 transitions have been identified and attributed to 16 species including organic Oxygen-, Nitrogen-, Sulfur-bearing molecules and their isotopologues. Four dense cores MM7, MM8, MM4, and MM11 are line rich sources. Modeling of these spectral lines reveals the rotational temperature in a range of 72$-$115~K, 100$-$163~K, 102$-$204~K, and 84$-$123~K for the MM7, MM8, MM4, and MM11, respectively. The molecular column densities are 1.6 $\times$ 10$^{15}$ $-$ 9.2 $\times$ 10$^{17}$~cm$^{-2}$ toward the four cores. The cores MM8 and MM4 show chemical difference between Oxygen- and Nitrogen-bearing species, i.e., MM4 is rich in oxygen-bearing molecules while nitrogen-bearing molecules especially vibrationally excited HC$_{3}$N lines are mainly observed in MM8. The distinct initial temperature at accretion phase may lead to this N/O differentiation. Through analyzing column densities and spatial distributions of O-bearing Complex Organic Molecules (COMs), we found that C$_{2}$H$_{5}$OH and CH$_{3}$OCH$_{3}$ might have a common precursor, CH$_{3}$OH. CH$_{3}$OCHO and CH$_{3}$OCH$_{3}$ are likely chemically linked. In addition, the observed variation in HC$_{3}$N and HC$_{5}$N emission may indicate that their different formation mechanism at hot and cold regions. Comment: 40 pages, 23 figures |
| نوع الوثيقة: | Working Paper |
| DOI: | 10.1093/mnras/stac624 |
| URL الوصول: | http://arxiv.org/abs/2203.12255 |
| رقم الأكسشن: | edsarx.2203.12255 |
| قاعدة البيانات: | arXiv |
| DOI: | 10.1093/mnras/stac624 |
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