The ALMA-ATOMS survey: Vibrationally excited HC<sub>3</sub>N lines in hot cores

doi:10.1051/0004-6361/202452598

	The ALMA-ATOMS survey: Vibrationally excited HC₃N lines in hot cores
	Chen, Li 1; Qin, Sheng-Li 1; Liu, Tie 2; Goldsmith, Paul F.3; Liu, Xunchuan 2; Peng, Yaping 4; Tang, Xindi5,6 ; Garay, Guido 7,8; Kou, Zhiping 1,5,9; Tang, Mengyao 10; Sanhueza, Patricio 11,12,13; Li, Zi-Yang 1,2; Gorai, Prasanta 14,15; Das, Swagat R.7; Bronfman, Leonardo 7; Dewangan, Lokesh 16; Garcia, Pablo 8,17; Li, Shanghuo 18; Lee, Chang Won 19,20; Liu, Hong-Li 1; Toth, L. Viktor 21,22; Chibueze, James O.23,24,25; Hwang, Jihye 19; Li, Xiaohu5,6 ; Xu, Fengwei 26,27; Zou, Jiahang 1,2; Jiao, Wenyu 2; Zhang, Zhenying 1,2; Zhang, Yong28
	2025-02-11
Source Publication	ASTRONOMY & ASTROPHYSICS
ISSN	0004-6361
Volume	694 Pages:A166
Contribution Rank	5
Abstract	Context. Interstellar molecules are excellent tools for studying the physical and chemical environments of massive star-forming regions. In particular, the vibrationally excited HC3N (HC3N) lines are the key tracers for probing hot cores environments. Aims. We present the Atacama Large Millimeter/submillimeter Array (ALMA) 3 mm observations of HC3N lines in 60 hot cores and investigate how the physical conditions affect the excitation of HC3N* transitions. Methods. We used the XCLASS for line identification. Under the assumption of local thermodynamic equilibrium, we derived the rotation temperature and column density of HC3N* transitions in hot cores. Additionally, we calculated the H-2 column density and number density, along with the abundance of HC3N* relative to H-2, to enable a comparison of the physical properties of hot cores with different numbers of HC3N* states. Results. We have detected HC3N* lines in 52 hot cores, 29 of which show more than one vibrationally excited state. Hot cores with higher gas temperatures have more detections of these vibrationally excited lines. The excitation of HC3N* requires dense environments, and its spatial distribution is affected by the presence of UC HII regions. The observed column density of HC3N* contributes to the number of HC3N* states in hot-core environments. Conclusions. After analyzing the various factors influencing HC3N* excitation in hot cores, we conclude that the excitation of HC3N* is mainly driven by mid-IR pumping, while collisional excitation is ineffective.
Keyword	stars: formation ISM: abundances HII regions ISM: molecules
DOI	10.1051/0004-6361/202452598
Indexed By	SCI
Language	英语
WOS Keyword	STAR-FORMING REGIONS ; MASSIVE STAR ; 3-MILLIMETER OBSERVATIONS ; CHEMICAL EVOLUTION ; ORION ; SUBMILLIMETER ; CYANOACETYLENE ; MILLIMETER ; HNCO ; TURBULENCE
Funding Project	National Key R&D Program of China[2022YFA1603100] ; National Natural Science Foundation of China (NSFC)[12033005] ; National Natural Science Foundation of China (NSFC)[12073061] ; National Natural Science Foundation of China (NSFC)[12122307] ; Xinjiang Uygur Autonomous Region ; National Aeronautics and Space Administration[80NM0018D0004] ; National Aeronautics and Space Administration[FB210003] ; NSFC[12203011] ; Yunnan Provincial Department of Science and Technology[202101BA070001-261] ; Yunnan Provincial Department of Science and Technology[JP22H01271] ; Yunnan Provincial Department of Science and Technology[JP23H01221] ; JSPS ; Yoshinori Ohsumi Fund (Yoshinori Ohsumi Award for Fundamental Research) ; Fondecyt Postdoctoral fellowship[FB210003] ; Fondecyt Postdoctoral fellowship[3220162] ; Basic Science Research Program through the NRF - Ministry of Education, Science and Technology[NRF-2019R1A2C1010851] ; Korea Astronomy and Space Science Institute - Korea government (MSIT)[2024-1-841-00] ; Yunnan Fundamental Research Project[202301AT070118] ; Yunnan Fundamental Research Project[202401AS070121] ; Xingdian Talent Support Plan-Youth Project ; Natural Science Foundation of Xinjiang Uygur Autonomous Region[2024D01E37] ; National Science Foundation of China[12473025] ; Chinese Academy of Sciences (CAS) ; CAS South America Center for Astronomy (CAS-SACA) in Santiago, Chile ; ALMA[2019.1.00685]
WOS Research Area	Astronomy & Astrophysics
WOS Subject	Astronomy & Astrophysics
WOS ID	WOS:001418747000031
Publisher	EDP SCIENCES S A
Funding Organization	National Key R&D Program of China ; National Natural Science Foundation of China (NSFC) ; Xinjiang Uygur Autonomous Region ; National Aeronautics and Space Administration ; NSFC ; Yunnan Provincial Department of Science and Technology ; JSPS ; Yoshinori Ohsumi Fund (Yoshinori Ohsumi Award for Fundamental Research) ; Fondecyt Postdoctoral fellowship ; Basic Science Research Program through the NRF - Ministry of Education, Science and Technology ; Korea Astronomy and Space Science Institute - Korea government (MSIT) ; Yunnan Fundamental Research Project ; Xingdian Talent Support Plan-Youth Project ; Natural Science Foundation of Xinjiang Uygur Autonomous Region ; National Science Foundation of China ; Chinese Academy of Sciences (CAS) ; CAS South America Center for Astronomy (CAS-SACA) in Santiago, Chile ; ALMA
Citation statistics	Cited Times:2[WOS] [WOS Record] [Related Records in WOS]
Document Type	期刊论文
Identifier	http://ir.xao.ac.cn/handle/45760611-7/7449
Collection	射电天文研究室_恒星形成与演化研究团组
Corresponding Author	Chen, Li; Qin, Sheng-Li; Liu, Tie
Affiliation	1.Yunnan Univ, Sch Phys & Astron, Kunming 650091, Peoples R China 2.Chinese Acad Sci, Shanghai Astron Observ, 80 Nandan Rd, Shanghai 200030, Peoples R China 3.CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA 4.Kunming Univ Sci & Technol, Fac Sci, Dept Phys, Kunming 650500, Peoples R China 5.Chinese Acad Sci, Xinjiang Astron Observ, 150 Sci 1 St, Urumqi 830011, Xinjiang, Peoples R China 6.Xinjiang Key Lab Radio Astrophys, 150 Sci 1 St, Urumqi 830011, Xinjiang, Peoples R China 7.Univ Chile, Dept Astron, Santiago 7591245, Chile 8.Chinese Acad Sci, CAS, Natl Astron Observ, South Amer Ctr Astron, Beijing 100101, Peoples R China 9.IHEP, Beijing 100049, Peoples R China 10.Chuxiong Normal Univ, Inst Astrophys, Sch Phys & Elect Sci, Chuxiong 675000, Peoples R China 11.Inst Sci Tokyo, Dept Earth & Planetary Sci, Tokyo 1528551, Japan 12.Natl Inst Nat Sci, Natl Astron Observ Japan, 2-21-1 Osawa, Tokyo 1818588, Japan 13.SOKENDAI, Grad Univ Adv Studies, Dept Astron Sci, 2-21-1 Osawa, Tokyo 1818588, Japan 14.Univ Oslo, Rosseland Ctr Solar Phys, POB 1029, N-0315 Oslo, Norway 15.Univ Oslo, Inst Theoret Astrophys, POB 1029, N-0315 Oslo, Norway 16.PHYS RES LAB, Ahmadabad 380009, India 17.Univ Catolica Norte, Inst Astron, Antofagasta, Chile 18.Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany 19.Korea Astron & Space Sci Inst, 776 Daedeokdaero, Daejeon 34055, South Korea 20.Korea Univ Sci & Technol UST, 217 Gajeong Ro, Daejeon 34113, South Korea 21.Eotvos Lorand Univ, Dept Astron, Pazmany Peter Setany 1-A, H-1117 Budapest, Hungary 22.Univ Debrecen, Fac Sci & Technol, Egyetemter 1, H-4032 Debrecen, Hungary 23.Univ South Africa, Dept Math Sci, Wet Rd & Pioneer Ave, ZA-1709 Florida Pk, Roodepoort, South Africa 24.North West Univ, Ctr Space Res, Potchefstroom Campus,Private Bag X6001, ZA-2520 Potchefstroom, South Africa 25.Univ Nigeria, Fac Phys Sci, Dept Phys & Astron, Carver Bldg,1 Univ Rd, Nsukka 410001, Nigeria 26.Univ Cologne, Phys Inst 1, Zulpicher Str 77, D-50937 Cologne, Germany 27.Peking Univ, Inst Microelect, 5 Yiheyuan Rd, Beijing 100871, Peoples R China 28.Sun Yat Sen Univ, Sch Phys & Astron, 2 Daxue Rd, Zhuhai 519082, Guangdong, Peoples R China
Recommended Citation GB/T 7714	Chen, Li,Qin, Sheng-Li,Liu, Tie,et al. The ALMA-ATOMS survey: Vibrationally excited HC₃N lines in hot cores[J]. ASTRONOMY & ASTROPHYSICS,2025,694:A166.
APA	Chen, Li.,Qin, Sheng-Li.,Liu, Tie.,Goldsmith, Paul F..,Liu, Xunchuan.,...&Zhang, Yong.(2025).The ALMA-ATOMS survey: Vibrationally excited HC₃N lines in hot cores.ASTRONOMY & ASTROPHYSICS,694,A166.
MLA	Chen, Li,et al."The ALMA-ATOMS survey: Vibrationally excited HC₃N lines in hot cores".ASTRONOMY & ASTROPHYSICS 694(2025):A166.

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