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ALMA Survey of Orion Planck Galactic Cold Clumps (ALMASOP): A Forming Quadruple System with Continuum "Ribbons" and Intricate Outflows

dc.contributorShanghai Astronomical Observatory, Chinese Academy of Sciences, 80 Nandan Road, Shanghai 200030, People's Republic of China; School of Astronomy and Space Sciences, University of Chinese Academy of Sciences, No. 19A Yuquan Road, Beijing 100049, People's Republic of China
dc.contributorShanghai Astronomical Observatory, Chinese Academy of Sciences, 80 Nandan Road, Shanghai 200030, People's Republic of China
dc.contributorDepartment of Physics and Astronomy, Saint Mary's College of California, 1928 Saint Mary's Road, Moraga, CA 94575, USA
dc.contributorDepartment of Astronomy, University of Texas Austin, Austin, TX 78712, USA
dc.contributorNRC Herzberg Astronomy and Astrophysics, 5071 West Saanich Road, Victoria, BC, V9E 2E7, Canada; Department of Physics and Astronomy, University of Victoria, 3800 Finnerty Road, Elliot Building, Victoria, BC, V8P 5C2, Canada
dc.contributorDepartment of Physics, P.O. Box 64, FI-00014, University of Helsinki, Finland
dc.contributorJet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109, USA
dc.contributorDepartment of Astronomy, Yunnan University, Kunming 650091, People's Republic of China
dc.contributorNational Astronomical Observatory of Japan, National Institutes of Natural Sciences, 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan; Department of Astronomical Science, SOKENDAI (The Graduate University for Advanced Studies), 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan
dc.contributorDepartment of Astronomy, School of Physics, Peking University, Beijing 100871, People's Republic of China; Kavli Institute for Astronomy and Astrophysics, Peking University, Haidian District, Beijing 100871, People's Republic of China
dc.contributorNobeyama Radio Observatory, National Astronomical Observatory of Japan, National Institutes of Natural Sciences, Nobeyama, Minamimaki, Minamisaku, Nagano 384-1305, Japan; Astronomical Science Program, Graduate Institute for Advanced Studies, SOKENDAI,2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan
dc.contributorAcademia Sinica Institute of Astronomy and Astrophysics, 11F of AS/NTU Astronomy-Mathematics Building, No.1, Sec. 4, Roosevelt Rd, Taipei 10617, Taiwan
dc.contributorInstitute of Astronomy and Department of Physics, National Tsing Hua University, Hsinchu, Taiwan
dc.contributorMax Planck Institute for Astronomy, Königstuhl 17, D-69117 Heidelberg, Germany
dc.contributorNational Astronomical Observatories, Chinese Academy of Sciences, A20 Datun Road, Chaoyang District, Beijing 100101, People's Republic of China
dc.contributorKorea Astronomy and Space Science Institute, 776 Daedeokdae-ro, Yuseong-gu, Daejeon 34055, Republic of Korea; University of Science and Technology, Korea (UST), 217 Gajeong-ro, Yuseong-gu, Daejeon 34113, Republic of Korea
dc.contributorAcademia Sinica Institute of Astronomy and Astrophysics, 11F of AS/NTU Astronomy-Mathematics Building, No.1, Sec. 4, Roosevelt Rd, Taipei 10617, Taiwan; Physical Research laboratory, Navrangpura, Ahmedabad, Gujarat 380009, India
dc.contributorDepartamento de Astronomía, Universidad de Chile, Las Condes, 7591245 Santiago, Chile
dc.contributorDepartment of Earth Science Education, Seoul National University, 1 Gwanak-ro, Gwanak-gu, Seoul 08826, Republic of Korea; SNU Astronomy Research Center, Seoul National University, 1 Gwanak-ro, Gwanak-gu, Seoul 08826, Republic of Korea
dc.contributorGemini Observatory/NSF's NOIRLab, 670 N. A'ohoku Place, Hilo, HI 96720, USA
dc.contributorArmagh Observatory and Planetarium, College Hill, Armagh, BT61 9DB, UK
dc.contributorNational Astronomical Observatories, Chinese Academy of Sciences, Datun Rd. A20, Beijing, People's Republic of China
dc.contributorJeremiah Horrocks Institute, UCLAN, Preston, PR1 2HE, UK
dc.contributor.authorLuo, Qiu-yi
dc.contributor.authorLiu, Tie
dc.contributor.authorLee, Aaron T.
dc.contributor.authorOffner, Stella S. R.
dc.contributor.authordi Francesco, James
dc.contributor.authorJohnstone, Doug
dc.contributor.authorJuvela, Mika
dc.contributor.authorGoldsmith, Paul F.
dc.contributor.authorQin, Sheng-Li
dc.contributor.authorMai, Xiaofeng
dc.contributor.authorLiu, Xun-chuan
dc.contributor.authorSanhueza, Patricio
dc.contributor.authorXu, Feng-Wei
dc.contributor.authorTatematsu, Ken'ichi
dc.contributor.authorDutta, Somnath
dc.contributor.authorChen, Huei-Ru Vivien
dc.contributor.authorLi, Shanghuo
dc.contributor.authorYang, Aiyuan
dc.contributor.authorLiu, Sheng-Yuan
dc.contributor.authorLee, Chin-Fei
dc.contributor.authorHirano, Naomi
dc.contributor.authorLee, Chang Won
dc.contributor.authorSahu, Dipen
dc.contributor.authorShang, Hsien
dc.contributor.authorHsu, Shih-Ying
dc.contributor.authorBronfman, Leonardo
dc.contributor.authorKwon, Woojin
dc.contributor.authorRawlings, M. G.
dc.contributor.authorEden, David
dc.contributor.authorLu, Xing
dc.contributor.authorGu, Qi-lao
dc.contributor.authorRen, Zhiyuan
dc.contributor.authorWard-Thompson, D.
dc.contributor.authorShen, Zhi-Qiang
dc.date.accessioned2024-02-01T17:10:20Z
dc.date.available2024-02-01T17:10:20Z
dc.date.issued2023-07-01T00:00:00Z
dc.identifier.doi10.3847/2041-8213/acdddf
dc.identifier.doi10.48550/arXiv.2306.07839
dc.identifier.other2023arXiv230607839L
dc.identifier.otherastro-ph.GA
dc.identifier.otherarXiv:2306.07839
dc.identifier.other2023arXiv230607839L
dc.identifier.other2023ApJ...952L...2L
dc.identifier.other10.3847/2041-8213/acdddf
dc.identifier.other10.48550/arXiv.2306.07839
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dc.identifier.urihttp://hdl.handle.net/20.500.14302/1343
dc.description.abstractOne of the most poorly understood aspects of low-mass star formation is how multiple-star systems are formed. Here we present the results of Atacama Large Millimeter/submillimeter Array (ALMA) Band 6 observations toward a forming quadruple protostellar system, G206.93-16.61E2, in the Orion B molecular cloud. ALMA 1.3 mm continuum emission reveals four compact objects, of which two are Class I young stellar objects and the other two are likely in prestellar phase. The 1.3 mm continuum emission also shows three asymmetric ribbon-like structures that are connected to the four objects, with lengths ranging from ~500 to ~2200 au. By comparing our data with magnetohydrodynamic simulations, we suggest that these ribbons trace accretion flows and also function as gas bridges connecting the member protostars. Additionally, ALMA CO J = 2-1 line emission reveals a complicated molecular outflow associated with G206.93-16.61E2, with arc-like structures suggestive of an outflow cavity viewed pole-on.
dc.publisherThe Astrophysical Journal
dc.titleALMA Survey of Orion Planck Galactic Cold Clumps (ALMASOP): A Forming Quadruple System with Continuum "Ribbons" and Intricate Outflows
dc.typearticle
dc.source.journalApJL
dc.source.journalApJL..952
dc.source.volume952
refterms.dateFOA2024-02-01T17:10:20Z
dc.identifier.bibcode2023ApJ...952L...2L


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