ATOMS: ALMA Three-millimeter Observations of Massive Star-forming regions - V. Hierarchical fragmentation and gas dynamics in IRDC G034.43+00.24

被引：1

作者：

Liu, Hong-Li ^{[1
]}

Tej, Anandmayee ^{[2
]}

Liu, Tie ^{[3
,4
]}

Issac, Namitha ^{[2
]}

Saha, Anindya ^{[2
]}

Goldsmith, Paul F. ^{[5
]}

Wang, Jun-Zhi ^{[3
,6
]}

Zhang, Qizhou ^{[7
]}

Qin, Sheng-Li ^{[1
]}

Wang, Ke ^{[8
,9
]}

Li, Shanghuo ^{[10
]}

Soam, Archana ^{[11
]}

Dewangan, Lokesh ^{[12
]}

Lee, Chang Won ^{[10
,13
]}

Li, Pak-Shing ^{[14
]}

Liu, Xun-Chuan ^{[9
]}

Zhang, Yong ^{[15
]}

Ren, Zhiyuan ^{[16
]}

Juvela, Mika ^{[17
]}

Bronfman, Leonardo ^{[18
]}

Wu, Yue-Fang ^{[8
,9
]}

Tatematsu, Ken'ichi ^{[19
]}

Chen, Xi ^{[20
]}

Li, Di ^{[16
,21
,22
]}

Stutz, Amelia ^{[23
,24
]}

Zhang, Siju ^{[8
]}

Toth, L. Viktor ^{[25
]}

Luo, Qiu-Yi ^{[3
]}

Xu, Feng-Wei ^{[8
,9
]}

Li, Jinzeng ^{[16
]}

Liu, Rong ^{[16
]}

Zhou, Jianwen ^{[16
]}

Zhang, Chao ^{[1
,26
]}

Tang, Mengyao ^{[1
,27
]}

Zhang, Chao ^{[1
,26
]}

Baug, Tapas ^{[28
]}

Mannfors, E. ^{[17
]}

Chakali, Eswaraiah ^{[16
,29
]}

Dutta, Somnath ^{[30
]}

机构：

[1] Yunnan Univ, Dept Astron, Kunming 650091, Yunnan, Peoples R China

[2] Indian Inst Space Sci & Technol, Thiruvananthapuram 695547, Kerala, India

[3] Chinese Acad Sci, Shanghai Astron Observ, 80 Nandan Rd, Shanghai 200030, Peoples R China

[4] Chinese Acad Sci, Shanghai Astron Observ, Key Lab Res Galaxies & Cosmol, 80 Nandan Rd, Shanghai 200030, Peoples R China

[5] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA

[6] Chinese Acad Sci, Key Lab Radio Astron, Nanjing 210008, Peoples R China

[7] Harvard & Smithsonian, Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA

[8] Peking Univ, Kavli Inst Astron & Astrophys, 5 Yiheyuan Rd, Beijing 100871, Peoples R China

[9] Peking Univ, Dept Astron, Beihing 100871, Peoples R China

[10] Korea Astron & Space Sci Inst, 776 Daedeokdaero, Daejeon 34055, South Korea

[11] NASA, SOFIA Sci Ctr, USRA, Ames Res Ctr, MS-12,N232, Moffett Field, MS USA

[12] Phys Res Lab, Ahmadabad 380009, Gujarat, India

[13] Univ Sci & Technol Korea UST, 217 Gajeong Ro, Daejeon 34113, South Korea

[14] Univ Calif Berkeley, Dept Astron, 601 Campbell Hall, Berkeley, CA 94720 USA

[15] Sun Yat Sen Univ, Sch Phys & Astron, 2 Daxue Rd, Zhuhai 519082, Guangdong, Peoples R China

[16] Chinese Acad Sci, Natl Astron Observ, Beijing 100101, Peoples R China

[17] Univ Helsinki, Dept Phys, POB 64, FI-00014 Helsinki, Finland

[18] Univ Chile, Dept Astron, Santiago, Chile

[19] Natl Inst Nat Sci, Natl Astron Observ Japan, 2-21-1 Osawa, Mitaka, Tokyo 1818588, Japan

[20] GuangZhou Univ, Ctr Astrophys, Guangzhou 510006, Peoples R China

[21] Univ Chinese Acad Sci, Beijing 100049, Peoples R China

[22] Univ KwaZulu Natal, NAOC UKZN Computat Astrophys Ctr, ZA-4000 Durban, South Africa

[23] Univ Concepcion, Dept Astron, Av Esteban Iturra S-N,160-C, Concepcion, Chile

[24] Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany

[25] Eotvos Lorand Univ, Dept Astron, Pazmany Petersetany 1-A, H-1117 Budapest, Hungary

[26] Taiyuan Normal Univ, Dept Phys, Jinzhong 030619, Peoples R China

[27] Chuxiong Normal Univ, Sch Phys & Elect Sci, Inst Astrophys, Chuxiong, Peoples R China

[28] Satyendra Nath Bose Natl Ctr Basic Sci, Block JD,Sect 3, Kolkata 700106, India

[29] Indian Inst Sci Educ & Res Tirupati, Karakambadi Rd,Mangalam PO, Tirupati 517507, Andhra Pradesh, India

[30] Acad Sinica, Inst Astron & Astrophys, Roosevelt Rd, Taipei 10617, Taiwan

来源：

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY | 2022年 / 510卷 / 04期

基金：

中国国家自然科学基金; 美国国家航空航天局; 新加坡国家研究基金会;

关键词：

stars: formation; stars: kinematics and dynamics; ISM: clouds; ISM: individual objects: G034.43+00.24; MOLECULAR OUTFLOWS; MAGNETIC-FIELDS; CLOUD; CLUMPS; DENSE; PROTOSTARS; ACCRETION; COLLAPSE; DRIVEN;

D O I：

10.1093/mnras/stab2757

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We present new 3-mm continuum and molecular lines observations from the ATOMS survey towards the massive protostellar clump, MM1, located in the filamentary infrared dark cloud (IRDC), G034.43+00.24 (G34). The lines observed are the tracers of either dense gas (e.g. HCO+/(HCO+)-C-13 J= 1-0) or outflows (e.g. CS J = 2-1). The most complete picture to date of seven cores in MM1 is revealed by dust continuum emission. These cores are found to be gravitationally bound, with virial parameter, alpha(vir) < 2. At least four outflows are identified in MM1 with a total outflowing mass of similar to 45 M-circle dot, and a total energy of 1 x 10(47) erg, typical of outflows from a B0-type star. Evidence of hierarchical fragmentation, where turbulence dominates over thermal pressure, is observed at both the cloud and the clump scales. This could be linked to the scale-dependent, dynamical mass inflow/accretion on clump and core scales. We therefore suggest that the G34 cloud could be undergoing a dynamical mass inflow/accretion process linked to the multiscale fragmentation, which leads to the sequential formation of fragments of the initial cloud, clumps, and ultimately dense cores, the sites of star formation.

引用

页码：5009 / 5022

页数：14

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