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ALMA Survey of Orion Planck Galactic Cold Clumps (ALMASOP): Evidence for a Molecular Jet Launched at an Unprecedented Early Phase of Protostellar Evolution
Dutta, Somnath1; Lee, Chin-Fei1; Hirano, Naomi1; Liu, Tie2,3; Johnstone, Doug4,5; Liu, Sheng-Yuan1; Tatematsu, Ken'ichi6,7; Goldsmith, Paul F.8; Sahu, Dipen1; Evans, Neal J.9; Sanhueza, Patricio7,10; Kwon, Woojin11,12; Qin, Sheng-Li13; Samal, Manash Ranjan14; Zhang, Qizhou15; Kim, Kee-Tae16,17; Shang, Hsien1; Lee, Chang Won16,17; Moraghan, Anthony1; Jhan, Kai-Syun1; Li, Shanghuo16; Lee, Jeong-Eun18; Traficante, Alessio19; Juvela, Mika20; Bronfman, Leonardo21; Eden, David22; Soam, Archana23; He JH(何金华)21,24,25; Liu, Hong-li13; Kuan, Yi-Jehng26; Pelkonen, Veli-Matti27; Luo, Qiuyi2; Yi, Hee-Weon16; Hsu, Shih-Ying1,28
发表期刊ASTROPHYSICAL JOURNAL
2022-06-01
卷号931期号:2
DOI10.3847/1538-4357/ac67a1
产权排序第24完成单位
收录类别SCI
摘要

Protostellar outflows and jets play a vital role in star formation as they carry away excess angular momentum from the inner disk surface, allowing the material to be transferred toward the central protostar. Theoretically, low-velocity and poorly collimated outflows appear from the beginning of the collapse at the first hydrostatic core (FHSC) stage. With growing protostellar core mass, high-density jets are launched, entraininf an outflow from the infalling envelope. Until now, molecular jets have been observed at high velocity (greater than or similar to 100 km s(-1)) in early Class 0 protostars. We, for the first time, detect a dense molecular jet in SiO emission with low velocity (similar to 4.2 km s(-1), deprojected similar to 24 km s(-1)) from source G208.89-20.04Walma (hereafter G208Walma) using ALMA Band 6 observations. This object has some characteristics of FHSCs, such as a small outflow/jet velocity, extended 1.3 mm continuum emission, and N2D+ line emission. Additional characteristics, however, are typical of early protostars: collimated outflow and SiO jet. The full extent of the outflow corresponds to a dynamical timescale of similar to 930(-100)(+200) yr. The spectral energy distribution also suggests a very young source having an upper limit of T-bol similar to 31 K and L-bol similar to 0.8 L-circle dot. We conclude that G208Walma is likely in the transition phase from FHSC to protostar, and the molecular jet has been launched within a few hundred years of initial collapse. Therefore, G208Walma may be the earliest object discovered in the protostellar phase with a molecular jet.

资助项目ALMA[2018.1.00302] ; Ministry of Science and Technology of Taiwan[MoST: 107-2119-M-001-040-MY3] ; Ministry of Science and Technology of Taiwan[110-2112-M-001-021-MY3] ; Academia Sinica[AS-IA-108-M01] ; Academia Sinica[MoST 109-2112-M-001-023] ; Academia Sinica[109-2112-M001-048] ; National Natural Science Foundation of China (NSFC)[12073061] ; National Natural Science Foundation of China (NSFC)[12122307] ; Chinese Academy of Sciences[114231KYSB20200009] ; Shanghai Pujiang Program[20PJ1415500] ; China Manned Space Project[CMS-CSST-2021-B06] ; National Aeronautics and Space Administration[80NM0018D0004] ; Basic Science Research Program through the National Research Foundation of Korea (NRF) - Ministry of Education, Science and Technology[NRF2019R1A2C1010851] ; National Research Council of Canada ; Natural Sciences and Engineering Research Council of Canada (NSERC) Discovery Grant ; National Natural Science Foundation of China[12033005] ; Ministry of Science and Technology (MoST) in Taiwan[109-2112-M-001-028and 110-2112-M-001-019] ; Ministry of Science and Technology (MoST) in Taiwan[18H01259] ; Japan Society for the Promotion of Science (JSPS)[ACE210002] ; Japan Society for the Promotion of Science (JSPS)[FB21000] ; Japan Society for the Promotion of Science (JSPS)[PID2020-115892GB-I00] ; Japan Society for the Promotion of Science (JSPS)[MCIN/AEI/10.13039/501100011033]
项目资助者ALMA[2018.1.00302] ; Ministry of Science and Technology of Taiwan[MoST: 107-2119-M-001-040-MY3, 110-2112-M-001-021-MY3] ; Academia Sinica[AS-IA-108-M01, MoST 109-2112-M-001-023, 109-2112-M001-048] ; National Natural Science Foundation of China (NSFC)[12073061, 12122307] ; Chinese Academy of Sciences[114231KYSB20200009] ; Shanghai Pujiang Program[20PJ1415500] ; China Manned Space Project[CMS-CSST-2021-B06] ; National Aeronautics and Space Administration[80NM0018D0004] ; Basic Science Research Program through the National Research Foundation of Korea (NRF) - Ministry of Education, Science and Technology[NRF2019R1A2C1010851] ; National Research Council of Canada ; Natural Sciences and Engineering Research Council of Canada (NSERC) Discovery Grant ; National Natural Science Foundation of China[12033005] ; Ministry of Science and Technology (MoST) in Taiwan[109-2112-M-001-028and 110-2112-M-001-019, 18H01259] ; Japan Society for the Promotion of Science (JSPS)[ACE210002, FB21000, PID2020-115892GB-I00, MCIN/AEI/10.13039/501100011033]
语种英语
学科领域天文学 ; 恒星与银河系
学科门类理学 ; 理学::天文学
文章类型Article
出版者IOP Publishing Ltd
出版地TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
ISSN0004-637X
URL查看原文
WOS记录号WOS:000804951000001
WOS研究方向Astronomy & Astrophysics
WOS类目Astronomy & Astrophysics
关键词[WOS]CLOUD CORES ; STAR-FORMATION ; COLLAPSE ; 1ST ; SIO ; OUTFLOWS ; PROTOSTARS ; ACCRETION ; ROTATION
引用统计
被引频次:4[WOS]   [WOS记录]     [WOS相关记录]
文献类型期刊论文
版本出版稿
条目标识符http://ir.ynao.ac.cn/handle/114a53/25208
专题其他
通讯作者Dutta, Somnath
作者单位1.Institute of Astronomy and Astrophysics, Academia Sinica, Roosevelt Road, Taipei 10617, Taiwan, R.O.C.; sdutta@asiaa.sinica.edu.tw, cflee@asiaa.sinica.edu.tw;
2.Shanghai Astronomical Observatory, Chinese Academy of Sciences, 80 Nandan Road, Shanghai 200030, People's Republic of China;
3.Key Laboratory for Research in Galaxies and Cosmology, Chinese Academy of Sciences, 80 Nandan Road, Shanghai 200030 People's Republic of China;
4.NRC Herzberg Astronomy and Astrophysics, 5071 West Saanich Road, Victoria, BC V9E 2E7, Canada;
5.Department of Physics and Astronomy, University of Victoria, Victoria, BC V8P 1A1, Canada;
6.Nobeyama Radio Observatory, National Astronomical Observatory of Japan, National Institutes of Natural Sciences, 462-2 Nobeyama, Minamimaki, Minamisaku, Nagano 384-1305, Japan;
7.Department of Astronomical Science, SOKENDAI (The Graduate University for Advanced Studies), 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan;
8.Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, CA 91109, USA;
9.Department of Astronomy, The University of Texas at Austin, 2515 Speedway, Stop C1400, Austin, TX 78712-1205, USA;
10.National Astronomical Observatory of Japan, National Institutes of Natural Sciences, 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan;
11.Department of Earth Science Education, Seoul National University, 1 Gwanak-ro, Gwanak-gu, Seoul 08826, Republic of Korea;
12.SNU Astronomy Research Center, Seoul National University, 1 Gwanak-ro, Gwanak-gu, Seoul 08826, Republic of Korea;
13.Department of Astronomy, Yunnan University, and Key Laboratory of Particle Astrophysics of Yunnan Province, Kunming, 650091, People's Republic of China;
14.Physical Research Laboratory, Navrangpura, Ahmedabad, Gujarat 380009, India;
15.Center for Astrophysics—Harvard & Smithsonian, 60 Garden Street, Cambridge, MA 02138, USA;
16.Korea Astronomy and Space Science Institute (KASI), 776 Daedeokdae-ro, Yuseong-gu, Daejeon 34055, Republic of Korea;
17.University of Science and Technology, Korea (UST), 217 Gajeong-ro, Yuseong-gu, Daejeon 34113, Republic of Korea;
18.School of Space Research, Kyung Hee University, Yongin-Si, Gyeonggi-Do 17104, Republic of Korea;
19.IAPS-INAF, via Fosso del Cavaliere 100, I-00133, Rome, Italy;
20.Department of Physics, P.O.Box 64, FI-00014, University of Helsinki, Finland;
21.Departamento de Astronomía, Universidad de Chile, Casilla 36-D, Santiago, Chile;
22.Armagh Observatory and Planetarium, College Hill, Armagh, BT61 9DB, UK;
23.SOFIA Science Center, Universities Space Research Association, NASA Ames Research Center, Moffett Field, CA 94035, USA;
24.Yunnan Observatories, Chinese Academy of Sciences, 396 Yangfangwang, Guandu District, Kunming, 650216, People's Republic of China;
25.Chinese Academy of Sciences, South America Center for Astronomy, National Astronomical Observatories, CAS, Beijing 100101, People's Republic of China;
26.Department of Earth Sciences, National Taiwan Normal University, Taipei, Taiwan, R.O.C. & Institute of Astronomy and Astrophysics, Academia Sinica, Roosevelt Road, Taipei 10617, Taiwan, R.O.C.;
27.Institut de Ciències del Cosmos, Universitat de Barcelona, IEEC-UB, Martí i Franquès 1, E-08028 Barcelona, Spain;
28.National Taiwan University (NTU), No. 1, Section 4, Roosevelt Road, Taipei 10617, Taiwan, R.O.C.
推荐引用方式
GB/T 7714
Dutta, Somnath,Lee, Chin-Fei,Hirano, Naomi,et al. ALMA Survey of Orion Planck Galactic Cold Clumps (ALMASOP): Evidence for a Molecular Jet Launched at an Unprecedented Early Phase of Protostellar Evolution[J]. ASTROPHYSICAL JOURNAL,2022,931(2).
APA Dutta, Somnath.,Lee, Chin-Fei.,Hirano, Naomi.,Liu, Tie.,Johnstone, Doug.,...&Hsu, Shih-Ying.(2022).ALMA Survey of Orion Planck Galactic Cold Clumps (ALMASOP): Evidence for a Molecular Jet Launched at an Unprecedented Early Phase of Protostellar Evolution.ASTROPHYSICAL JOURNAL,931(2).
MLA Dutta, Somnath,et al."ALMA Survey of Orion Planck Galactic Cold Clumps (ALMASOP): Evidence for a Molecular Jet Launched at an Unprecedented Early Phase of Protostellar Evolution".ASTROPHYSICAL JOURNAL 931.2(2022).
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