| ATOMS: ALMA three-millimetre observations of massive star-forming regions-XVII. High-mass star-formation through a large-scale collapse in IRAS 15394-5358 | |
Das, Swagat R1; Merello, Manuel1; Bronfman, Leonardo1; Liu, Tie2; Garay, Guido1,3; Stutz, Amelia4; Mardones, Diego1; Zhou, Jian-Wen5; Sanhueza, Patricio6,7,8; Liu, Hong-Li9; Vázquez-Semadeni, Enrique10; Gómez, Gilberto C10; Palau, Aina10; Tej, Anandmayee11; Xu, Feng-Wei12,13; Baug, Tapas14; Dewangan, Lokesh K15; He JH(何金华)1,3,16 ; Zhu, Lei3; Li, Shanghuo17,18; Juvela, Mika19; Saha, Anindya11; Issac, Namitha2; Hwang, Jihye20; Nazeer, Hafiz11; Toth, L Viktor21
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| 发表期刊 | MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
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| 2024-10-23 | |
| 卷号 | 534期号:4页码:3832-3852 |
| DOI | 10.1093/mnras/stae2275 |
| 产权排序 | 第16完成单位 |
| 收录类别 | SCI ; EI |
| 关键词 | stars: formation stars: kinematics and dynamics ISM: clouds ISM: individual objects: IRAS 15394-5358 |
| 摘要 | Hub-filament systems are considered as natural sites for high-mass star formation. Kinematic analysis of the surroundings of hub-filaments is essential to better understand high-mass star formation within such systems. In this work, we present a detailed study of the massive Galactic protocluster IRAS 15394-5358, using continuum and molecular line data from the ALMA three-millimetre observations of massive star-forming regions (ATOMS) survey. The 3 mm dust continuum map reveals the fragmentation of the massive (M=843 M-circle dot) clump into six cores. The core C-1A is the largest (radius = 0.04 pc), the most massive (M=157 M-circle dot), and lies within the dense central region, along with two smaller cores (M=7 and 3 M-circle dot). The fragmentation process is consistent with the thermal Jeans fragmentation mechanism and virial analysis shows that all the cores have small virial parameter values (alpha(vir)<<2), suggesting that the cores are gravitationally bound. The mass versus radius relation indicates that three cores can potentially form at least a single massive star. The integrated intensity map of (HCO+)-C-13 shows that the massive clump is associated with a hub-filament system, where the central hub is linked with four filaments. A sharp velocity gradient is observed towards the hub, suggesting a global collapse where the filaments are actively feeding the hub. We discuss the role of global collapse and the possible driving mechanisms for the massive star formation activity in the protocluster. |
| 资助项目 | Fondecyt Postdoctoral fellowship[3220162]; ANID BASAL project[FB210003]; Fondecyt Regular[1220610]; Yunnan Fundamental Research Project[202301AT070118]; Yunnan Fundamental Research Project[202401AS070121]; UNAM-PAPIIT[IG100223]; Sistema Nacional de Investigadores of CONAHCyT; CONAHCyT[86372]; Chinese Academy of Sciences (CAS); Research Council of Finland[348342]; Research Council of Finland[2019.1.00685]; JSPS[JP22H01271]; JSPS[JP23H01221] |
| 项目资助者 | Fondecyt Postdoctoral fellowship[3220162] ; ANID BASAL project[FB210003] ; Fondecyt Regular[1220610] ; Yunnan Fundamental Research Project[202301AT070118, 202401AS070121] ; UNAM-PAPIIT[IG100223] ; Sistema Nacional de Investigadores of CONAHCyT ; CONAHCyT[86372] ; Chinese Academy of Sciences (CAS) ; Research Council of Finland[348342] ; Research Council of Finland[2019.1.00685] ; JSPS[JP22H01271, JP23H01221] |
| 语种 | 英语 |
| 学科领域 | 天文学 ; 恒星与银河系 |
| 文章类型 | Article |
| 出版者 | OXFORD UNIV PRESS |
| 出版地 | GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND |
| ISSN | 0035-8711 |
| URL | 查看原文 |
| WOS记录号 | WOS:001340463100008 |
| WOS研究方向 | Astronomy & Astrophysics |
| WOS类目 | Astronomy & Astrophysics |
| 关键词[WOS] | FILAMENTARY MOLECULAR CLOUDS ; GALACTIC PLANE SURVEY ; HIERARCHICAL FRAGMENTATION ; HOT CORES ; TEMPERATURE STRUCTURE ; JEANS FRAGMENTATION ; UNIVERSAL NURSERY ; ACCRETION FLOWS ; COMPLETE SAMPLE ; MAGNETIC-FIELD |
| EI入藏号 | 20244417298283 |
| EI主题词 | Kinematics |
| EI分类号 | 1301.1.1 - 1301.1.3 - 1302 - 1302.1.2 - 1303 |
| 引用统计 | |
| 文献类型 | 期刊论文 |
| 版本 | 出版稿 |
| 条目标识符 | http://ir.ynao.ac.cn/handle/114a53/27664 |
| 专题 | 其他 |
| 作者单位 | 1.Departamento de Astronomıá, Universidad de Chile, Las Condes, 7591245 Santiago, Chile; 2.Shanghai Astronomical Observatory, Chinese Academy of Sciences, 80 Nandan Road, Shanghai 200030, China; 3.Chinese Academy of Sciences South America Center for Astronomy, National Astronomical Observatories, CAS, Beijing 100101, China; 4.Departamento de Astronomıá, Universidad de Concepción, Av. Esteban Iturra s/n, Distrito Universitario 160-C, Chile; 5.Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, D-53121 Bonn, Germany; 6.Department of Earth and Planetary Sciences, Institute of Science, Tokyo, Meguro, Tokyo, 152-8551, Japan; 7.National Astronomical Observatory of Japan, National Institutes of Natural Sciences, 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan; 8.Astronomical Science Program, The Graduate University for Advanced Studies, SOKENDAI, 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan; 9.School of Physics and Astronomy, Yunnan University, Kunming 650091, P. R. China; 10.Instituto de Radioastronomía y Astrofísica, Universidad Nacional Autónoma de México, Apdo. Postal 3-72, Morelia, Michoacán 58089, México; 11.Department of Earth & Space Sciences, Indian Institute of Space Science and Technology, Thiruvananthapuram 695 547, Kerala, India; 12.Kavli Institute for Astronomy and Astrophysics, Peking University, Beijing 100871, P. R. China; 13.Department of Astronomy, School of Physics, Peking University, Beijing 100871, P. R. China; 14.S. N. Bose National Centre for Basic Sciences, Block-JD, Sector-III, Salt Lake City, Kolkata 700106, India; 15.Physical Research Laboratory, Navrangpura, Ahmedabad 380 009, India; 16.Yunnan Observatories, Chinese Academy of Sciences, 396 Yang-fangwang, Guandu District, Kunming 650216, P. R. China; 17.Max Planck Institute of Astronomy, Königstuhl 17, D-69117 Heidelberg, Germany; 18.SOFIA Science Centre, USRA, NASA Ames Research Centre, MS-12, N232, Moffett Field, CA 94035, USA; 19.Department of Physics, University of Helsinki, PO Box 64, FI-00014 Helsinki, Finland; 20.Korea Astronomy and Space Science Institute, 776 Daedeokdaero, Yuseong-gu, Daejeon 34055, Republic of Korea; 21.Institute of Physics and Astronomy, Eotvos Lorand University, Pazmany Peter setany 1/A, H-1117 Budapest, Hungary |
| 推荐引用方式 GB/T 7714 | Das, Swagat R,Merello, Manuel,Bronfman, Leonardo,et al. ATOMS: ALMA three-millimetre observations of massive star-forming regions-XVII. High-mass star-formation through a large-scale collapse in IRAS 15394-5358[J]. MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY,2024,534(4):3832-3852. |
| APA | Das, Swagat R.,Merello, Manuel.,Bronfman, Leonardo.,Liu, Tie.,Garay, Guido.,...&Toth, L Viktor.(2024).ATOMS: ALMA three-millimetre observations of massive star-forming regions-XVII. High-mass star-formation through a large-scale collapse in IRAS 15394-5358.MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY,534(4),3832-3852. |
| MLA | Das, Swagat R,et al."ATOMS: ALMA three-millimetre observations of massive star-forming regions-XVII. High-mass star-formation through a large-scale collapse in IRAS 15394-5358".MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY 534.4(2024):3832-3852. |
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| ATOMS_ ALMA three-mi（4717KB） | 期刊论文 | 出版稿 | 开放获取 | CC BY-NC-SA | 浏览 请求全文 | |
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