YNAO OpenIR  > 其他
ATOMS: ALMA Three-millimeter Observations of Massive Star-forming regions - XI. From inflow to infall in hub-filament systems
Zhou, Jian-Wen1,2; Liu, Tie3; II, Neal J Evans,4; Garay, Guido5; Goldsmith, Paul F6; Gómez, Gilberto C7; Vázquez-Semadeni, Enrique7; Liu, Hong-Li8; Stutz, Amelia M9; Wang, Ke10; Juvela, Mika11; He JH(何金华)12,13,14; Li, Di1,2,15; Bronfman, Leonardo14; Liu, Xunchuan3; Xu, Feng-Wei10,16; Tej, Anandmayee17; Dewangan, L K18; Li, Shanghuo19; Zhang, Siju10; Zhang, Chao20; Ren, Zhiyuan1; Tatematsu, Ken’ichi21,22; Li, Pak Shing23; Lee, Chang Won19,24; Baug, Tapas25; Qin, Sheng-Li8; Wu, Yuefang16; Peng, Yaping26; Zhang, Yong27,28,29; Liu, Rong1,2; Luo, Qiu-Yi2,3; Ge, Jixing13; Saha, Anindya17; Chakali, Eswaraiah30; Zhang, Qizhou31; Kim, Kee-Tae19; Ristorcelli, Isabelle32; Shen, Zhi-Qiang3; Li, Jin-Zeng1
Source PublicationMONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
2022-07-13
Volume514Issue:4Pages:6038-6052
DOI10.1093/mnras/stac1735
Contribution Rank第12完成单位
Indexed BySCI ; EI
KeywordISM: clouds ISM: Hii regions ISM: kinematics and dynamics stars: formation stars: protostars
Abstract

We investigate the presence of hub-filament systems in a large sample of 146 active proto-clusters, using (HCO+)-C-13 J = 1-0 molecular line data obtained from the ATOMS survey. We find that filaments are ubiquitous in proto-clusters, and hub-filament systems are very common from dense core scales (similar to 0.1 pc) to clump/cloud scales (similar to 1-10 pc). The proportion of proto-clusters containing hub-filament systems decreases with increasing dust temperature (T-d) and luminosity-to-mass ratios (L/M) of clumps, indicating that stellar feedback from H ii regions gradually destroys the hub-filament systems as proto-clusters evolve. Clear velocity gradients are seen along the longest filaments with a mean velocity gradient of 8.71 km s(-1) pc(-1) and a median velocity gradient of 5.54 km s(-1) pc(-1). We find that velocity gradients are small for filament lengths larger than similar to 1 pc, probably hinting at the existence of inertial inflows, although we cannot determine whether the latter are driven by large-scale turbulence or large-scale gravitational contraction. In contrast, velocity gradients below similar to 1 pc dramatically increase as filament lengths decrease, indicating that the gravity of the hubs or cores starts to dominate gas infall at small scales. We suggest that self-similar hub-filament systems and filamentary accretion at all scales may play a key role in high-mass star formation.

Funding ProjectNational Natural Science Foundation of China (NSFC)[12073061] ; National Natural Science Foundation of China (NSFC)[12122307] ; National Natural Science Foundation of China (NSFC)[12103045] ; Chinese Academy of Sciences[114231KYSB20200009] ; Shanghai Pujiang Program[20PJ1415500] ; China Manned Space Project[CMS-CSST-2021-B06] ; China Manned Space Project[CMS-CSST-2021-A09] ; China Manned Space Project[CMS-CSST-2021-A10] ; National Natural Science Foundation of China[11988101] ; National Natural Science Foundation of China[12033005] ; National Natural Science Foundation of China[11873086] ; National Natural Science Foundation of China[U1631237] ; National Research Foundation of Korea (NRF) - Ministry of Education, Science and Technology[NRF-2019R1A2C1010851] ; CONACYT grant[255295] ; National Aeronautics and Space Administration[80NM0018D0004] ; Chinese Academy of Sciences (CAS) ; ANID BASAL projects[ACE210002] ; ANID BASAL projects[FB210003] ; UNAM-PAPIIT[IN103822] ; NSFC[11988101] ; NSFC[E013430201] ; NSFC[11725313] ; NSFC[11403041] ; NSFC[11373038] ; NSFC[11373045] ; NSFC[U1931117] ; China Postdoctoral Science Foundation[2021M700248] ; JSPS KAKENHI[20H05645] ; S. N. Bose National Centre for Basic Sciences under the Department of Science and Technology (DST), Government of India ; National Science Foundation of China (NSFC)[11973099] ; f Ramanujan Fellowship by Science and Engineering Research Board (SERB), Department of Science and Technology (DST), Govt. of India[RJF/2020/000071]
Funding OrganizationNational Natural Science Foundation of China (NSFC)[12073061, 12122307, 12103045] ; Chinese Academy of Sciences[114231KYSB20200009] ; Shanghai Pujiang Program[20PJ1415500] ; China Manned Space Project[CMS-CSST-2021-B06, CMS-CSST-2021-A09, CMS-CSST-2021-A10] ; National Natural Science Foundation of China[11988101, 12033005, 11873086, U1631237] ; National Research Foundation of Korea (NRF) - Ministry of Education, Science and Technology[NRF-2019R1A2C1010851] ; CONACYT grant[255295] ; National Aeronautics and Space Administration[80NM0018D0004] ; Chinese Academy of Sciences (CAS) ; ANID BASAL projects[ACE210002, FB210003] ; UNAM-PAPIIT[IN103822] ; NSFC[11988101, E013430201, 11725313, 11403041, 11373038, 11373045, U1931117] ; China Postdoctoral Science Foundation[2021M700248] ; JSPS KAKENHI[20H05645] ; S. N. Bose National Centre for Basic Sciences under the Department of Science and Technology (DST), Government of India ; National Science Foundation of China (NSFC)[11973099] ; f Ramanujan Fellowship by Science and Engineering Research Board (SERB), Department of Science and Technology (DST), Govt. of India[RJF/2020/000071]
Language英语
Subject Area天文学 ; 恒星与银河系 ; 恒星形成与演化
MOST Discipline Catalogue理学 ; 理学::天文学
SubtypeArticle
PublisherOXFORD UNIV PRESS
Publication PlaceGREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
ISSN0035-8711
URL查看原文
WOS IDWOS:000825725300011
WOS Research AreaAstronomy & Astrophysics
WOS SubjectAstronomy & Astrophysics
WOS KeywordMOLECULAR CLOUD EVOLUTION ; UNIVERSAL NURSERY ; TRAO SURVEY ; ACCRETION ; FRAGMENTATION ; COLLAPSE ; DYNAMICS ; OUTFLOW ; GRAVITY ; FLOWS
EI Accession Number20223112473684
EI KeywordsVelocity
EI Classification Number657.2 Extraterrestrial Physics and Stellar Phenomena
Citation statistics
Cited Times:9[WOS]   [WOS Record]     [Related Records in WOS]
Document Type期刊论文
Version出版稿
Identifierhttp://ir.ynao.ac.cn/handle/114a53/25335
Collection其他
Corresponding AuthorZhou, Jian-Wen; Liu, Tie
Affiliation1.National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100101, People’s Republic of China;
2.School of Astronomy and Space Science, University of Chinese Academy of Sciences, Beijing 100049, People’s Republic of China;
3.Shanghai Astronomical Observatory, Chinese Academy of Sciences, 80 Nandan Road, Shanghai 200030, People’s Republic of China;
4.Department of Astronomy, The University of Texas at Austin, 2515 Speedway, Stop C1400, Austin, TX 78712-1205, USA;
5.Departamento de Astronomıa, Universidad de Chile, Camino el Observatorio 1515, Las Condes, Santiago, Chile;
6.Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, CA 91109, USA;
7.Instituto de Radioastronomía y Astrofísica, Universidad Nacional Autónoma de México, Antigua Carretera a Pátzcuaro # 8701, Ex-Hda. San José de la Huerta, Morelia, Michoacán, C.P. 58089, México;
8.Department of Astronomy, Yunnan University, Kunming 650091, People’s Republic of China;
9.Departamento de Astronomía, Universidad de Concepción, Casilla 160-C, Concepción, Chile;
10.Kavli Institute for Astronomy and Astrophysics, Peking University, Haidian District, Beijing 100871, People’s Republic of China;
11.Department of Physics, University of Helsinki, PO Box 64, FI-00014 Helsinki, Finland;
12.Yunnan Observatories, Chinese Academy of Sciences, 396 Yangfangwang, Guandu District, Kunming 650216, People’s Republic of China;
13.Chinese Academy of Sciences South America Center for Astronomy, National Astronomical Observatories, CAS, Beijing 100101, People’s Republic of China;
14.Departamento de Astronomía, Universidad de Chile, Casilla 36-D, Santiago, Chile;
15.NAOC-UKZN Computational Astrophysics Centre, University of KwaZulu-Natal, Durban 4000, South Africa;
16.Department of Astronomy, School of Physics, Peking University, Beijing 100871, People’s Republic of China;
17.Indian Institute of Space Science and Technology, Thiruvananthapuram, Kerala 695547, India;
18.Physical Research Laboratory, Navrangpura, Ahmedabad 380009, India;
19.Korea Astronomy and Space Science Institute, 776 Daedeokdae-ro, Yuseong-gu, Daejeon 34055, Republic of Korea;
20.Institute of Astronomy and Astrophysics, Anqing Normal University, Anqing 246133, People’s Republic of China;
21.Nobeyama Radio Observatory, National Astronomical Observatory of Japan, National Institutes of Natural Sciences, Nobeyama, Minamimaki, Minamisaku, Nagano 384-1305, Japan;
22.Department of Astronomical Science, The Graduate University for Advanced Studies, SOKENDAI, 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan;
23.Astronomy Department, University of California, Berkeley, CA 94720, USA;
24.University of Science and Technology, Korea (UST), 217 Gajeong-ro, Yuseong-gu, Daejeon 34113, Republic of Korea;
25.S. N. Bose National Centre for Basic Sciences, JD Block, Sector-III, Salt Lake City, Kolkata 700106, India;
26.College of Science, Yunnan Agricultural University, Kunming 650201, People’s Republic of China;
27.School of Physics and Astronomy, Sun Yat-sen University, 2 Daxue Road, Tangjia, Zhuhai, Guangdong Province, People’s Republic of China;
28.CSST Science Center for the Guangdong-Hongkong-Macau Greater Bay Area, Sun Yat-Sen University, Guangdong Province, People’s Republic of China;
29.Laboratory for Space Research, The University of Hong Kong, Hong Kong 000000, People’s Republic of China;
30.Indian Institute of Science Education and Research (IISER) Tirupati, Rami Reddy Nagar, Karakambadi Road, Mangalam (P.O.), Tirupati 517507, India;
31.Center for Astrophysics, Harvard Smithsonian, 60 Garden Street, Cambridge, MA 02138, USA;
32.IRAP, Université de Toulouse, CNRS, UPS, CNES, Toulouse 31400, France
Recommended Citation
GB/T 7714
Zhou, Jian-Wen,Liu, Tie,II, Neal J Evans,,et al. ATOMS: ALMA Three-millimeter Observations of Massive Star-forming regions - XI. From inflow to infall in hub-filament systems[J]. MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY,2022,514(4):6038-6052.
APA Zhou, Jian-Wen.,Liu, Tie.,II, Neal J Evans,.,Garay, Guido.,Goldsmith, Paul F.,...&Li, Jin-Zeng.(2022).ATOMS: ALMA Three-millimeter Observations of Massive Star-forming regions - XI. From inflow to infall in hub-filament systems.MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY,514(4),6038-6052.
MLA Zhou, Jian-Wen,et al."ATOMS: ALMA Three-millimeter Observations of Massive Star-forming regions - XI. From inflow to infall in hub-filament systems".MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY 514.4(2022):6038-6052.
Files in This Item:
File Name/Size DocType Version Access License
ATOMS_ ALMA Three-mi(6700KB)期刊论文出版稿开放获取CC BY-NC-SAView Application Full Text
Related Services
Recommend this item
Bookmark
Usage statistics
Export to Endnote
Google Scholar
Similar articles in Google Scholar
[Zhou, Jian-Wen]'s Articles
[Liu, Tie]'s Articles
[II, Neal J Evans,]'s Articles
Baidu academic
Similar articles in Baidu academic
[Zhou, Jian-Wen]'s Articles
[Liu, Tie]'s Articles
[II, Neal J Evans,]'s Articles
Bing Scholar
Similar articles in Bing Scholar
[Zhou, Jian-Wen]'s Articles
[Liu, Tie]'s Articles
[II, Neal J Evans,]'s Articles
Terms of Use
No data!
Social Bookmark/Share
File name: ATOMS_ ALMA Three-millimeter Observations of Massive Star-forming regions - XI. From inflow to infall in hub-filament systems.pdf
Format: Adobe PDF
All comments (0)
No comment.
 

Items in the repository are protected by copyright, with all rights reserved, unless otherwise indicated.