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The Serpens filament at the onset of slightly supercritical collapse
Gong, Y.1,2,3; Li, G. X.4,5; Mao, R. Q.2,3; Henkel, C.1,6,7; Menten, K. M.1; Fang, M.8; Wang, M.2,3; Sun, J. X.2,3
2018-11-28
Source PublicationASTRONOMY & ASTROPHYSICS
ISSN1432-0746
Volume620Pages:19
Corresponding AuthorGong, Y.(ygong@mpifr-bonn.mpg.de)
AbstractThe Serpens filament, as one of the nearest infrared dark clouds, is regarded as a pristine filament at a very early evolutionary stage of star formation. In order to study its molecular content and dynamical state, we mapped this filament in seven species: (CO)-O-18, HCO+, HNC, HCN, N2H+, CS, and CH3OH. Among them, HCO+, HNC, HCN, and CS show self-absorption, while (CO)-O-18 is most sensitive to the filamentary structure. A kinematic analysis demonstrates that this filament forms a velocity-coherent (trans) sonic structure, a large part of which is one of the most quiescent regions in the Serpens cloud. Widespread (CO)-O-18 depletion is found throughout the Serpens filament. Based on the Herschel dust-derived H-2 column density map, the line mass of the filament is 36-41 M-circle dot pc(-1), and its full width at half maximum is 0.17 +/- 0.01 pc, while its length is approximate to 1.6 pc. The inner radial column density profile of this filament can be well fitted with a Plummer profile with an exponent of 2.2 +/- 0.1, a scale radius of 0.018 +/- 0.003 pc, and a central density of (4.0 +/- 0.8) x 10(4) cm(-3). The Serpens filament appears to be slightly supercritical. The widespread blue-skewed HNC and CS line profiles and HCN hyperfine line anomalies across this filament indicate radial infall in parts of the Serpens filament. (CO)-O-18 velocity gradients also indicate accretion flows along the filament. The velocity and density structures suggest that such accretion flows are likely due to a longitudinal collapse parallel to the filament's long axis. Both the radial infall rate (similar to 72 M-circle dot Myr(-1), inferred from HNC and CS blue-skewed profiles) and the longitudinal accretion rate (similar to 10 M-circle dot Myr(-1), inferred from (CO)-O-18 velocity gradients) along the Serpens filament are lower than all previously reported values in other filaments. This indicates that the Serpens filament lies at an early evolutionary stage when collapse has just begun, or that thermal and nonthermal support are effective in providing support against gravity.
KeywordISM: clouds ISM: molecules radio lines: ISM line: profiles ISM: kinematics and dynamics
DOI10.1051/0004-6361/201833583
WOS KeywordSTAR-FORMATION ; DARK ; CLOUDS ; MASS ; HERSCHEL ; CORES ; FRAGMENTATION ; PERSEUS ; HCN ; SIMULATIONS
Indexed BySCI
Language英语
WOS Research AreaAstronomy & Astrophysics
WOS SubjectAstronomy & Astrophysics
WOS IDWOS:000451412000001
PublisherEDP SCIENCES S A
Citation statistics
Cited Times:1[WOS]   [WOS Record]     [Related Records in WOS]
Document Type期刊论文
Identifierhttp://libir.pmo.ac.cn/handle/332002/20721
Collection中国科学院紫金山天文台
Corresponding AuthorGong, Y.
Affiliation1.Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany
2.Chinese Acad Sci, Purple Mt Observ, 2 West Beijing Rd, Nanjing 210008, Peoples R China
3.Chinese Acad Sci, Key Lab Radio Astron, 2 West Beijing Rd, Nanjing 210008, Peoples R China
4.Univ Observ Munich, Scheinerstr 1, D-81679 Munich, Germany
5.Yunnan Univ, South Western Inst Astron Res, Kunming 650500, Yunnan, Peoples R China
6.King Abdulaziz Univ, Fac Sci, Dept Astron, POB 80203, Jeddah 21589, Saudi Arabia
7.Chinese Acad Sci, Xinjiang Astron Observ, Urumqi 830011, Peoples R China
8.Univ Arizona, Dept Astron, 933 North Cherry Ave, Tucson, AZ 85721 USA
Recommended Citation
GB/T 7714
Gong, Y.,Li, G. X.,Mao, R. Q.,et al. The Serpens filament at the onset of slightly supercritical collapse[J]. ASTRONOMY & ASTROPHYSICS,2018,620:19.
APA Gong, Y..,Li, G. X..,Mao, R. Q..,Henkel, C..,Menten, K. M..,...&Sun, J. X..(2018).The Serpens filament at the onset of slightly supercritical collapse.ASTRONOMY & ASTROPHYSICS,620,19.
MLA Gong, Y.,et al."The Serpens filament at the onset of slightly supercritical collapse".ASTRONOMY & ASTROPHYSICS 620(2018):19.
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