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http://dx.doi.org/10.5467/JKESS.2018.39.6.519

Kinematics of the Northern Filament in Orion Molecular Clouds Complex Using 12CO Molecular Observation Data  

Jo, Hoon (Department of Earth Science Education, Korea National University of Education)
Sohn, Jungjoo (Department of Earth Science Education, Korea National University of Education)
Kim, ShinYoung (Korea Astronomy and Space Science Institute)
Lee, JeeWon (Korea Astronomy and Space Science Institute)
Kim, Sungsoo S. (Department of Astronomy & Space Science, Kyung Hee University)
Morris, Mark (Department of Physics & Astronomy, UCLA)
Publication Information
Journal of the Korean earth science society / v.39, no.6, 2018 , pp. 519-532 More about this Journal
Abstract
We investigated the effect of galactic plane toward molecular motion and kinematics in the northern filament (NF) of Orion Molecular Clouds Complex (OMC) using $^{12}CO$ (J=1-0) line. Observed data were from three areas including NF1, NF2, and NF3 in far-out order from galactic plane, for a total 270 hours by Seoul National University Radio Astronomy Observatory (SRAO) 6m telescope, with 2arcmin spatial resolution. galactic plane and OMC NF were connected to each other along the magnetic field at a density of 3% for $^{12}CO$ (J=2-1) and 9% for the case of dust. $^{12}CO$ (J=1-0), $^{12}CO$ (J=2-1), and interstellar dusts were distributed uniformly in NF3, but only in certain regions with relatively high density in NF1 and NF2. NF showed a single structure, partial shrinking motion in NF1, and rotational motion at the bottom of NF2, and spiral rotation associated with magnetic field only in NF3. The position-velocity analysis showed that the materials including $^{12}CO$ (J=1-0) could flow toward galactic plane along NF2 and NF3. However, there was no clear cause for the material to flow toward galactic plane in this result. Further detailed observation for rotational motion at the top of NF1 and NF2 might help to confirm it.
Keywords
Orion Molecular Clouds Complex (OMC); filament; galactic plane; $^{12}CO$ line;
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