Chemistry of Protostellar Clumps in the High-mass, Star-forming Filamentary Infrared Dark Cloud G034.43+00.24

doi:10.3847/1538-4357/abadfe

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	Chemistry of Protostellar Clumps in the High-mass, Star-forming Filamentary Infrared Dark Cloud G034.43+00.24
	Liu, Hong-Li 7; Sanhueza, Patricio 8,9; Liu, Tie 10; Zavagno, Annie 1,2; Tang, Xin-Di 3,4; Wu, Yuefang 5,6; Zhang, Siju 1
刊名	ASTROPHYSICAL JOURNAL
	2020-09-01
卷号	901 期号:1 页码:31
关键词	Astrochemistry Chemical abundances Interstellar medium Interstellar molecules Star formation
ISSN号	0004-637X
DOI	10.3847/1538-4357/abadfe
产权排序	7
英文摘要	To search for the potential chemical dependence on physical conditions, we have carried out the study of chemistry on the nine protostellar clumps of the high-mass star-forming infrared dark cloud G034.43+00.24, with observations of several similar to 1 mm lines by the Atacama Pathfinder EXperiment telescope. They include CO/(CO)-C-13/(CO)-O-18(2-1), HCO+/(HCO+)-C-13(3-2), HCN/(HCN)-C-13(3-2), HNC (3-2), CS/(CS)-S-34(5-4), SiO.(6 -5), SO(6-5), p-H2CO.(3-2), and CH3OH.(5-4). All the clumps are simply grouped into two classes: highluminosity protostellar clumps (MM1-MM4, L-bol > similar to 103 L-circle dot) and low-luminosity protostellar clumps (MM5-MM9, L-bol << 10(3) L-circle dot). Our observations indicate that (CO)-C-13 suffers either no or low depletion in the clump environment of G034.43+00.24 as characterized by a nearly constant level of the (CO)-C-13 abundance distribution. For the remaining relatively dense gas tracers, we find that their abundances tend to get enhanced in the highluminosity protostellar clumps as opposed to the low-luminosity counterparts. We suggest that for most, if not all, of the dense gas tracers the high abundance mainly arises from both the high luminosities and associated outflows of the high-luminosity protostellar clumps while the low abundance could be due to the lack of such active starforming activities in the low-luminosity protostellar clumps.
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资助项目	Fondecyt[3190161] ; Japan Society for the Promotion of Science (JSPS)[18H01259] ; NSFC[11903070] ; NSFC[11433008] ; Heaven Lake Hundred-Talent Program of Xinjiang Uygur Autonomous Region of PR China
WOS关键词	CHEMICAL EVOLUTION ; MOLECULAR OUTFLOWS ; ABUNDANCE RATIO ; INTERSTELLAR ; EMISSION ; GAS ; FORMALDEHYDE ; POPULATION ; PRECURSORS ; REGIONS
WOS研究方向	Astronomy & Astrophysics
语种	英语
出版者	IOP PUBLISHING LTD
WOS记录号	WOS:000573465800001
资助机构	Fondecyt ; Japan Society for the Promotion of Science (JSPS) ; NSFC ; Heaven Lake Hundred-Talent Program of Xinjiang Uygur Autonomous Region of PR China
内容类型	期刊论文
源URL	[http://ir.xao.ac.cn/handle/45760611-7/3670]
专题	恒星形成与演化研究团组
通讯作者	Liu, Hong-Li
作者单位	1.Aix Marseille Univ, CNRS, CNES, LAM, Marseille, France 2.Inst Univ France IUF, Paris, France 3.Chinese Acad Sci, Xinjiang Astron Observ, Urumqi 830011, Peoples R China 4.Chinese Acad Sci, Key Lab Radio Astron, Urumqi 830011, Peoples R China 5.Peking Univ, Sch Phys, Astron Dept, 5 Yi He Yuan Rd, Beijing 100871, Peoples R China 6.Peking Univ, Kavli Inst Astron & Astrophys, 5 Yi He Yuan Rd, Beijing 100871, Peoples R China 7.Univ Concepcion, Dept Astron, Av Esteban Iturra S-N,160-C, Concepcion, Chile 8.Natl Inst Nat Sci, Natl Astron Observ Japan, 2-21-1 Osawa, Mitaka, Tokyo 1818588, Japan 9.SOKENDAI Grad Univ Adv Studies, Dept Astron Sci, 2-21-1 Osawa, Mitaka, Tokyo 1818588, Japan 10.Chinese Acad Sci, Shanghai Astron Observ, 80 Nandan Rd, Shanghai 200030, Peoples R China
推荐引用方式 GB/T 7714	Liu, Hong-Li,Sanhueza, Patricio,Liu, Tie,et al. Chemistry of Protostellar Clumps in the High-mass, Star-forming Filamentary Infrared Dark Cloud G034.43+00.24[J]. ASTROPHYSICAL JOURNAL,2020,901(1):31.
APA	Liu, Hong-Li.,Sanhueza, Patricio.,Liu, Tie.,Zavagno, Annie.,Tang, Xin-Di.,...&Zhang, Siju.(2020).Chemistry of Protostellar Clumps in the High-mass, Star-forming Filamentary Infrared Dark Cloud G034.43+00.24.ASTROPHYSICAL JOURNAL,901(1),31.
MLA	Liu, Hong-Li,et al."Chemistry of Protostellar Clumps in the High-mass, Star-forming Filamentary Infrared Dark Cloud G034.43+00.24".ASTROPHYSICAL JOURNAL 901.1(2020):31.