Kinetic temperature of massive star-forming molecular clumps measured with formaldehyde: V. The massive filament DR21

doi:10.1051/0004-6361/202449352

	Kinetic temperature of massive star-forming molecular clumps measured with formaldehyde: V. The massive filament DR21
	Zhao, X.1,2; Tang, X. D.1,2,3,4 ; Henkel, C.1,5; Gong, Y.5,6; Lin, Y.5,7; Li, D. L.1,2,3,4 ; He, Y. X.1,2,3,4 ; Ao, Y. P.6; Lu, X.8; Liu, T.8; Sun, Y.6; Wang, K.9 ; Chen, X. P.6; Esimbek, J.1,3,4 ; Zhou, J. J.1,3,4 ; Wu, J. W.2,10; Qiu, J. J.11; Zheng, X. W.12; Li, J. S.1,2; Luo, C. S.1,2; Zhao, Q.1,2
	2024-07-12
Source Publication	ASTRONOMY & ASTROPHYSICS
ISSN	0004-6361
Volume	687 Pages:A207
Contribution Rank	1
Abstract	The kinetic temperature structure of the massive filament DR21 within the Cygnus X molecular cloud complex has been mapped using the IRAM 30 m telescope. This mapping employed the para-H2CO triplet (J(KaKc) = 3(03)-2(02), 3(22)-2(21), and 3(21)-2(20)) on a scale of similar to 0.1 pc. By modeling the averaged line ratios of para-H2CO 3(22)-2(21)/3(03)-2(02) and 3(21)-2(20)/3(03) -2(02) with RADEX under non local thermodynamic equilibrium (LTE) assumptions, the kinetic temperature of the dense gas was derived, which ranges from 24 to 114 K, with an average temperature of 48.3 +/- 0.5 K at a density of n(H-2)= 10(5) cm(-3). In comparison to temperature measurements using NH3 (1, 1)/(2,2) and far-infrared (FIR) wavelengths, the para-H2CO(3-2) lines reveal significantly higher temperatures. The dense clumps in various regions appear to correlate with the notable kinetic temperature (T-kin greater than or similar to 50 K) of the dense gas traced by H2CO. Conversely, the outskirts of the DR21 filament display lower temperature distributions (T-kin < 50 K). Among the four dense cores (N44, N46, N48, and N54), temperature gradients are observed on a scale of similar to 0.1-0.3 pc. This suggests that the warm dense gas traced by H2CO is influenced by internal star formation activity. With the exception of the dense core N54, the temperature profiles of these cores were fitted with power-law indices ranging from -0.3 to -0.5, with a mean value of approximately -0.4. This indicates that the warm dense gas probed by H2CO is heated by radiation emitted from internally embedded protostar(s) and/or clusters. While there is no direct evidence supporting the idea that the dense gas is heated by shocks resulting from a past explosive event in the DR21 region on a scale of similar to 0.1 pc, our measurements of H2CO toward the DR21W1 region provide compelling evidence that the dense gas in this specific area is indeed heated by shocks originating from the western DR21 flow. Higher temperatures as traced by H2CO appear to be associated with turbulence on a scale of similar to 0.1 pc. The physical parameters of the dense gas as determined from H2CO lines in the DR21 filament exhibit aremarkable similarity to the results obtained in OMC-1 and N113, albeit on a scale of approximately 0.1-0.4 pc. This may imply that the physical mechanisms governing the dynamics and thermodynamics of dense gas traced by H2CO in diverse star formation regions may be dominated by common underlying principles despite variations in specific environmental conditions.
Keyword	stars: formation stars: massive ISM: clouds ISM: molecules
DOI	10.1051/0004-6361/202449352
Indexed By	SCI
Language	英语
WOS Keyword	H-II REGIONS ; DR-21 OUTFLOW SOURCE ; GALACTIC-CENTER ; PHYSICAL-PROPERTIES ; DENSE GAS ; CHEMICAL COMPLEXITY ; METHANOL MASERS ; THERMAL BALANCE ; SCALE STRUCTURE ; SURVEY AMMONIA
Funding Project	National Key R&D Program of China[2023YFA1608002] ; National Key R&D Program of China[2022YFA1603103] ; Chinese Academy of Sciences (CAS) Light of West China Program[xbzg-zdsys-202212] ; Tianshan Talent Program of Xinjiang Uygur Autonomous Region[2022TSYCLJ0005] ; Natural Science Foundation of Xinjiang Uygur Autonomous Region[2022D01E06] ; Regional Collaborative Innovation Project of Xinjiang Uyghur Autonomous Region[2022E01050] ; Regional Collaborative Innovation Project of Xinjiang Uyghur Autonomous Region[2022D01A359] ; CAS Light of West China Program[2020-XBQNXZ-017] ; National Natural Science Foundation of China[12173075] ; National Natural Science Foundation of China[12373029] ; Xinjiang Key Laboratory of Radio Astrophysics[2023D04033] ; Youth Innovation Promotion Association CAS ; Tianchi Talent Program of Xinjiang Uygur Autonomous Region ; Chinese Academy of Sciences President' s International Fellowship Initiative[2023VMA0031] ; Chinese Academy of Sciences President' s International Fellowship Initiative[2025PVA0048]
WOS Research Area	Astronomy & Astrophysics
WOS Subject	Astronomy & Astrophysics
WOS ID	WOS:001270377500005
Publisher	EDP SCIENCES S A
Funding Organization	National Key R&D Program of China ; Chinese Academy of Sciences (CAS) Light of West China Program ; Tianshan Talent Program of Xinjiang Uygur Autonomous Region ; Natural Science Foundation of Xinjiang Uygur Autonomous Region ; Regional Collaborative Innovation Project of Xinjiang Uyghur Autonomous Region ; CAS Light of West China Program ; National Natural Science Foundation of China ; Xinjiang Key Laboratory of Radio Astrophysics ; Youth Innovation Promotion Association CAS ; Tianchi Talent Program of Xinjiang Uygur Autonomous Region ; Chinese Academy of Sciences President' s International Fellowship Initiative
Citation statistics	Cited Times:5[WOS] [WOS Record] [Related Records in WOS]
Document Type	期刊论文
Identifier	http://ir.xao.ac.cn/handle/45760611-7/6887
Collection	射电天文研究室_恒星形成与演化研究团组
Corresponding Author	Tang, X. D.
Affiliation	1.Chinese Acad Sci, Xinjiang Astron Observ, Urumqi 830011, Peoples R China 2.Univ Chinese Acad Sci, Beijing 100080, Peoples R China 3.Chinese Acad Sci, Key Lab Radio Astron, Urumqi 830011, Peoples R China 4.Xinjiang Key Lab Radio Astrophys, Urumqi 830011, Peoples R China 5.Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany 6.Chinese Acad Sci, Purple Mt Observ, Nanjing 210008, Peoples R China 7.Max Planck Inst Extraterr Phys, Giessenbachstr 1, D-85748 Garching, Germany 8.Chinese Acad Sci, Shanghai Astron Observ, 80 Nandan Rd, Shanghai 200030, Peoples R China 9.Peking Univ, Kavli Inst Astron & Astrophys, Beijing 100871, Peoples R China 10.Chinese Acad Sci, Natl Astron Observ, Beijing 100101, Peoples R China 11.Jinggangshan Univ, Sch Math & Phys, Jian 343009, Peoples R China 12.Nanjing Univ, Sch Astron & Space Sci, Nanjing 210093, Peoples R China
First Author Affilication	Xinjiang Astronomical Observatory, Chinese Academy of Sciences
Corresponding Author Affilication	Xinjiang Astronomical Observatory, Chinese Academy of Sciences
Recommended Citation GB/T 7714	Zhao, X.,Tang, X. D.,Henkel, C.,et al. Kinetic temperature of massive star-forming molecular clumps measured with formaldehyde: V. The massive filament DR21[J]. ASTRONOMY & ASTROPHYSICS,2024,687:A207.
APA	Zhao, X..,Tang, X. D..,Henkel, C..,Gong, Y..,Lin, Y..,...&Zhao, Q..(2024).Kinetic temperature of massive star-forming molecular clumps measured with formaldehyde: V. The massive filament DR21.ASTRONOMY & ASTROPHYSICS,687,A207.
MLA	Zhao, X.,et al."Kinetic temperature of massive star-forming molecular clumps measured with formaldehyde: V. The massive filament DR21".ASTRONOMY & ASTROPHYSICS 687(2024):A207.

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