ATOMS: ALMA Three-millimeter Observations of Massive Star-forming regions - XV. Steady accretion from global collapse to core feeding in massive hub-filament system SDC335

被引：45

作者：

Xu, Feng-Wei ^{[1
,2
]}

Wang, Ke ^{[1
]}

Liu, Tie ^{[3
]}

Goldsmith, Paul F. ^{[4
]}

Zhang, Qizhou ^{[5
]}

Juvela, Mika ^{[6
]}

Liu, Hong-Li ^{[7
]}

Qin, Sheng-Li ^{[7
]}

Li, Guang-Xing ^{[8
]}

Tej, Anandmayee ^{[9
]}

Garay, Guido ^{[10
]}

Bronfman, Leonardo ^{[10
]}

Li, Shanghuo ^{[11
]}

Wu, Yue-Fang ^{[1
,2
]}

Gomez, Gilberto C. ^{[12
]}

Vazquez-Semadeni, Enrique ^{[12
]}

Tatematsu, Ken'ichi ^{[13
]}

Ren, Zhiyuan ^{[14
]}

Zhang, Yong ^{[15
]}

Toth, L. Viktor ^{[16
]}

Liu, Xunchuan ^{[3
]}

Yue, Nannan ^{[1
]}

Zhang, Siju ^{[1
]}

Baug, Tapas ^{[17
]}

Issac, Namitha ^{[18
]}

Stutz, Amelia M. ^{[19
]}

Liu, Meizhu ^{[7
]}

Fuller, Gary A. ^{[20
,21
]}

Tang, Mengyao ^{[22
]}

Zhang, Chao ^{[23
]}

Dewangan, Lokesh ^{[24
]}

Lee, Chang Won ^{[11
,25
]}

Zhou, Jianwen ^{[14
]}

Xie, Jinjin ^{[3
]}

Jiao, Wenyu ^{[1
,2
]}

Wang, Chao ^{[1
,2
]}

Liu, Rong ^{[14
]}

Luo, Qiuyi ^{[3
]}

Soam, Archana

Eswaraiah, Chakali ^{[26
]}

机构：

[1] Peking Univ, Kavli Inst Astron & Astrophys, 5 Yi Heyuan Rd, Beijing 100871, Peoples R China

[2] Peking Univ, Sch Phys, Dept Astron, Beijing 100871, Peoples R China

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

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

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

[6] Univ Helsinki, Dept Phys, FI-00014 Helsinki, Finland

[7] Yunnan Univ, Sch Phys & Astron, Kunming 650091, Peoples R China

[8] Yunnan Univ, South Western Inst Astron Res, Kunming, Peoples R China

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

[10] Univ Chile, Dept Astron, Santiago 7591245, Chile

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

[12] Univ Nacl Autonoma Mexico, Inst Radioastron & Astrofis, Apdo Postal 3-72, Morelia 58089, Michoacan, Mexico

[13] Natl Astron Observ Japan, Natl Inst Nat Sci, Nobeyama Radio Observ, Minamisaku, Nagano 3841305, Japan

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

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

[16] Eotvos Lorand Univ, Dept Astron, Pazmany Peter Setany1-A, H-1117 Budapest, Hungary

[17] SN Bose Natl Ctr Basic Sci, Block JD,Sect 3, Kolkata 700106, India

[18] Indian Inst Astrophys, 2 Block, Bengaluru 560034, India

[19] Univ Concepcion, Dept Astron, Casilla160-C, Concepcion, Chile

[20] Univ Manchester, Jodrell Bank Ctr Astrophys, Sch Nat Sci, Dept Phys & Astron, Manchester, England

[21] Univ Cologne, I Phys Inst, Zulpicher Str77, D-50937 Cologne, Germany

[22] Chuxiong Normal Univ, Inst Astrophys, Sch Phys & Elect Sci, Chuxiong 675000, Peoples R China

[23] Anqing Normal Univ, Inst Astron & Astrophys, Anqing 246133, Peoples R China

[24] Phys Res Lab, Ahmadabad 380009, India

[25] Univ Sci & Technol, Korea UST, 217 Gajeongro, Daejeon 34113, South Korea

[26] Indian Inst Sci Educ & Res IISER Tirupati, Karakambadi Rd, Tirupati 517507, India

来源：

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY | 2023年 / 520卷 / 03期

基金：

新加坡国家研究基金会; 美国国家科学基金会; 美国国家航空航天局; 中国国家自然科学基金; 国家重点研发计划;

关键词：

stars: formation; stars: protostars; ISM: kinematics and dynamics; ISM: individual object: SDC335; INFRARED DARK CLOUD; SCALE GREATER-THAN-OR-EQUAL-TO-10 PC; COMPACT SOURCE CATALOG; HIERARCHICAL FRAGMENTATION; HOT CORES; HI-GAL; GRAVITATIONAL COLLAPSE; PHYSICAL-PROPERTIES; VELOCITY-COHERENT; MOLECULAR CLOUDS;

D O I：

10.1093/mnras/stad012

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We present ALMA Band-3/7 observations towards "the Heart' of a massive hub-filament system (HFS) SDC335, to investigate its fragmentation and accretion. At a resolution of similar to 0.03 pc, 3 mm continuum emission resolves two massive dense cores MM1 and MM2, with 383((+234)(-120)) M-? (10-24 % mass of "the Heart') and 74((+47)(-24))M-?, respectively. With a resolution down to 0.01 pc, 0.87 mm continuum emission shows MM1 further fragments into six condensations and multi-transition lines of H2CS provide temperature estimation. The relation between separation and mass of condensations at a scale of 0.01 pc favors turbulent Jeans fragmentation where the turbulence seems to be scale-free rather than scale-dependent. We use the (HCO+)-C-13 J = 1 - 0 emission line to resolve the complex gas motion inside "the Heart' in position-position-velocity space. We identify four major gas streams connected to large-scale filaments, inheriting the anti-clockwise spiral pattern. Along these streams, gas feeds the central massive core MM1. Assuming an inclination angle of 45(+/- 15)degrees and a (HCO+)-C-13 abundance of 5(+/- 3) x 10(-11), the total mass infall rate is estimated to be 2.40(+/- 0.78) x 10(-3) M-? yr(-1), numerically consistent with the accretion rates derived from the clump-scale spherical infall model and the core-scale outflows. The consistency suggests a continuous, near steady-state, and efficient accretion from global collapse, therefore ensuring core feeding. Our comprehensive study of SDC335 showcases the detailed gas kinematics in a prototypical massive infalling clump, and calls for further systematic and statistical studies in a large sample.

引用

页码：3259 / 3285

页数：27

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