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Wu, Jintai; Qiu, Keping; Poidevin, Frédérick; Bastien, Pierre; Liu, Junhao; Ching, Tao-Chung; Bourke, Tyler L.; Ward-Thompson, Derek; Pattle, Kate; Johnstone, Doug; Koch, Patrick M.; Arzoumanian, Doris; Lee, Chang Won; Fanciullo, Lapo; Onaka, Takashi; Hwang, Jihye; Le Gouellec, Valentin J. M.; Soam, Archana; Tamura, Motohide; Tahani, Mehrnoosh; Eswaraiah, Chakali; Li, Hua-Bai; Berry, David; Furuya, Ray S.; Coudé, Simon; Kwon, Woojin; Lin, Sheng-Jun; Wang, Jia-Wei; Hasegawa, Tetsuo; Lai, Shih-Ping; Byun, Do-Young; Chen, Zhiwei; Chen, Huei-Ru Vivien; Chen, Wen Ping; Chen, Mike; Cho, Jungyeon; Choi, Youngwoo; Choi, Yunhee; Choi, Minho; Chrysostomou, Antonio; Chung, Eun Jung; Dai, Sophia; Di Francesco, James; Diep, Pham Ngoc; Doi, Yasuo; Duan, Hao-Yuan; Duan, Yan; Eden, David; Fiege, Jason; Fissel, Laura M.; Franzmann, Erica; Friberg, Per; Friesen, Rachel; Fuller, Gary; Gledhill, Tim; Graves, Sarah; Greaves, Jane; Griffin, Matt; Gu, Qilao; Han, Ilseung; Hayashi, Saeko; Hoang, Thiem; Houde, Martin; Inoue, Tsuyoshi; Inutsuka, Shu-ichiro; Iwasaki, Kazunari; Jeong, Il-Gyo; Könyves, Vera; Kang, Ji-hyun; Kang, Miju; Karoly, Janik; Kataoka, Akimasa; Kawabata, Koji; Kim, Shinyoung; Kim, Mi-Ryang; Kim, Kyoung Hee; Kim, Kee-Tae; Kim, Jongsoo; Kim, Hyosung; Kim, Gwanjeong; Kirchschlager, Florian; Kirk, Jason; Kobayashi, Masato I. N.; Kusune, Takayoshi; Kwon, Jungmi; Lacaille, Kevin; Law, Chi-Yan; Lee, Hyeseung; Lee, Chin-Fei; Lee, Sang-Sung; Lee, Jeong-Eun; Li, Dalei; Li, Di; Li, Guangxing; Liu, Sheng-Yuan; Liu, Tie; Liu, Hong-Li; Lu, Xing; Lyo, A. -Ran; Mairs, Steve et al.
Bibliographical reference
The Astrophysical Journal
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2024
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Description
As part of the B-fields In Star-forming Region Observations survey, we present James Clerk Maxwell Telescope (JCMT) 850 μm polarimetric observations toward the Orion integral-shaped filament (ISF) that covers three portions known as OMC-1, OMC-2, and OMC-3. The magnetic field threading the ISF seen in the JCMT POL-2 map appears as a tale of three: pinched for OMC-1, twisted for OMC-2, and nearly uniform for OMC-3. A multiscale analysis shows that the magnetic field structure in OMC-3 is very consistent at all the scales, whereas the field structure in OMC-2 shows no correlation across different scales. In OMC-1, the field retains its mean orientation from large to small scales but shows some deviations at small scales. Histograms of relative orientations between the magnetic field and filaments reveal a bimodal distribution for OMC-1, a relatively random distribution for OMC-2, and a distribution with a predominant peak at 90∘ for OMC-3. Furthermore, the magnetic fields in OMC-1 and OMC-3 both appear to be aligned perpendicular to the fibers, which are denser structures within the filament, but the field in OMC-2 is aligned along with the fibers. All these suggest that gravity, turbulence, and magnetic field are each playing a leading role in OMC-1, 2, and 3, respectively. While OMC-2 and 3 have almost the same gas mass, density, and nonthermal velocity dispersion, there are on average younger and fewer young stellar objects in OMC-3, providing evidence that a stronger magnetic field will induce slower and less efficient star formation in molecular clouds.
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Two of the most fundamental questions in astrophysics are the conversion of molecular gas into stars and how this physical process is a function of environments on all scales, ranging from planetary systems, stellar clusters, galaxies to galaxy clusters. The main goal of this internal project is to get insight into the formation and evolution of
Helmut
Dannerbauer