Relative Velocities between 13CO Structures within 12CO Molecular Clouds
Velocity fields of molecular clouds (MCs) can provide crucial information on the merger and split between clouds, as well as their internal kinematics and maintenance, energy injection and redistribution, and even star formation within clouds. Using the CO spectral lines data from the Milky Way Imag...
| Main Authors: | , , , , , , , , , , , , |
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| Format: | Article |
| Language: | English |
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IOP Publishing
2024-01-01
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| Series: | The Astronomical Journal |
| Subjects: | |
| Online Access: | https://doi.org/10.3847/1538-3881/ad323a |
| _version_ | 1827288465907122176 |
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| author | Lixia Yuan Ji Yang Xuepeng Chen Yang Su Shaobo Zhang Xin Zhou Zhiwei Chen Qing-Zeng Yan Min Fang Fujun Du Yan Sun Hongchi Wang Ye Xu |
| author_facet | Lixia Yuan Ji Yang Xuepeng Chen Yang Su Shaobo Zhang Xin Zhou Zhiwei Chen Qing-Zeng Yan Min Fang Fujun Du Yan Sun Hongchi Wang Ye Xu |
| author_sort | Lixia Yuan |
| collection | DOAJ |
| description | Velocity fields of molecular clouds (MCs) can provide crucial information on the merger and split between clouds, as well as their internal kinematics and maintenance, energy injection and redistribution, and even star formation within clouds. Using the CO spectral lines data from the Milky Way Imaging Scroll Painting survey, we measure the relative velocities along the line of sight (Δ V _LOS ) between ^13 CO structures within ^12 CO MCs. Emphasizing MCs with double and triple ^13 CO structures, we find that approximately 70% of Δ V _LOS values are less than ∼1 km s ^−1 , and roughly 10% of values exceed 2 km s ^−1 , with a maximum of ∼5 km s ^−1 . Additionally, we compare Δ V _LOS with the internal velocity dispersion of ^13 CO structures ( ${\sigma }_{{}^{13}\mathrm{CO},\mathrm{in}}$ ) and find that about 40% of samples in either double or triple regime display distinct velocity discontinuities, i.e., the relative velocities between ^13 CO structures are larger than the internal line widths of ^13 CO structures. Among these 40% samples in the triple regime, 33% exhibit signatures of combinations through the two-body motion, whereas the remaining 7% show features of configurations through the multiple-body motion. The Δ V _LOS distributions for MCs with double and triple ^13 CO structures are similar, as well as their Δ V _LOS / ${\sigma }_{{}^{13}\mathrm{CO},\mathrm{in}}$ distributions. This suggests that relative motions of ^13 CO structures within MCs are random and independent of cloud complexities and scales. |
| first_indexed | 2024-04-24T11:32:24Z |
| format | Article |
| id | doaj.art-c476ac62de5f4c6e812eda620732bbf6 |
| institution | Directory Open Access Journal |
| issn | 1538-3881 |
| language | English |
| last_indexed | 2024-04-24T11:32:24Z |
| publishDate | 2024-01-01 |
| publisher | IOP Publishing |
| record_format | Article |
| series | The Astronomical Journal |
| spelling | doaj.art-c476ac62de5f4c6e812eda620732bbf62024-04-10T09:15:41ZengIOP PublishingThe Astronomical Journal1538-38812024-01-01167520710.3847/1538-3881/ad323aRelative Velocities between 13CO Structures within 12CO Molecular CloudsLixia Yuan0https://orcid.org/0000-0003-0804-9055Ji Yang1https://orcid.org/0000-0001-7768-7320Xuepeng Chen2https://orcid.org/0000-0003-3151-8964Yang Su3https://orcid.org/0000-0002-0197-470XShaobo Zhang4https://orcid.org/0000-0003-2549-7247Xin Zhou5https://orcid.org/0000-0003-2418-3350Zhiwei Chen6https://orcid.org/0000-0003-0849-0692Qing-Zeng Yan7https://orcid.org/0000-0003-4586-7751Min Fang8https://orcid.org/0000-0001-8060-1321Fujun Du9https://orcid.org/0000-0002-7489-0179Yan Sun10https://orcid.org/0000-0002-3904-1622Hongchi Wang11https://orcid.org/0000-0003-0746-7968Ye Xu12https://orcid.org/0000-0001-5602-3306Purple Mountain Observatory and Key Laboratory of Radio Astronomy, Chinese Academy of Sciences , 10 Yuanhua Road, Qixia District, Nanjing 210033, People’s Republic of China ; lxyuan@pmo.ac.cn, jiyang@pmo.ac.cnPurple Mountain Observatory and Key Laboratory of Radio Astronomy, Chinese Academy of Sciences , 10 Yuanhua Road, Qixia District, Nanjing 210033, People’s Republic of China ; lxyuan@pmo.ac.cn, jiyang@pmo.ac.cnPurple Mountain Observatory and Key Laboratory of Radio Astronomy, Chinese Academy of Sciences , 10 Yuanhua Road, Qixia District, Nanjing 210033, People’s Republic of China ; lxyuan@pmo.ac.cn, jiyang@pmo.ac.cnPurple Mountain Observatory and Key Laboratory of Radio Astronomy, Chinese Academy of Sciences , 10 Yuanhua Road, Qixia District, Nanjing 210033, People’s Republic of China ; lxyuan@pmo.ac.cn, jiyang@pmo.ac.cnPurple Mountain Observatory and Key Laboratory of Radio Astronomy, Chinese Academy of Sciences , 10 Yuanhua Road, Qixia District, Nanjing 210033, People’s Republic of China ; lxyuan@pmo.ac.cn, jiyang@pmo.ac.cnPurple Mountain Observatory and Key Laboratory of Radio Astronomy, Chinese Academy of Sciences , 10 Yuanhua Road, Qixia District, Nanjing 210033, People’s Republic of China ; lxyuan@pmo.ac.cn, jiyang@pmo.ac.cnPurple Mountain Observatory and Key Laboratory of Radio Astronomy, Chinese Academy of Sciences , 10 Yuanhua Road, Qixia District, Nanjing 210033, People’s Republic of China ; lxyuan@pmo.ac.cn, jiyang@pmo.ac.cnPurple Mountain Observatory and Key Laboratory of Radio Astronomy, Chinese Academy of Sciences , 10 Yuanhua Road, Qixia District, Nanjing 210033, People’s Republic of China ; lxyuan@pmo.ac.cn, jiyang@pmo.ac.cnPurple Mountain Observatory and Key Laboratory of Radio Astronomy, Chinese Academy of Sciences , 10 Yuanhua Road, Qixia District, Nanjing 210033, People’s Republic of China ; lxyuan@pmo.ac.cn, jiyang@pmo.ac.cnPurple Mountain Observatory and Key Laboratory of Radio Astronomy, Chinese Academy of Sciences , 10 Yuanhua Road, Qixia District, Nanjing 210033, People’s Republic of China ; lxyuan@pmo.ac.cn, jiyang@pmo.ac.cnPurple Mountain Observatory and Key Laboratory of Radio Astronomy, Chinese Academy of Sciences , 10 Yuanhua Road, Qixia District, Nanjing 210033, People’s Republic of China ; lxyuan@pmo.ac.cn, jiyang@pmo.ac.cnPurple Mountain Observatory and Key Laboratory of Radio Astronomy, Chinese Academy of Sciences , 10 Yuanhua Road, Qixia District, Nanjing 210033, People’s Republic of China ; lxyuan@pmo.ac.cn, jiyang@pmo.ac.cnPurple Mountain Observatory and Key Laboratory of Radio Astronomy, Chinese Academy of Sciences , 10 Yuanhua Road, Qixia District, Nanjing 210033, People’s Republic of China ; lxyuan@pmo.ac.cn, jiyang@pmo.ac.cnVelocity fields of molecular clouds (MCs) can provide crucial information on the merger and split between clouds, as well as their internal kinematics and maintenance, energy injection and redistribution, and even star formation within clouds. Using the CO spectral lines data from the Milky Way Imaging Scroll Painting survey, we measure the relative velocities along the line of sight (Δ V _LOS ) between ^13 CO structures within ^12 CO MCs. Emphasizing MCs with double and triple ^13 CO structures, we find that approximately 70% of Δ V _LOS values are less than ∼1 km s ^−1 , and roughly 10% of values exceed 2 km s ^−1 , with a maximum of ∼5 km s ^−1 . Additionally, we compare Δ V _LOS with the internal velocity dispersion of ^13 CO structures ( ${\sigma }_{{}^{13}\mathrm{CO},\mathrm{in}}$ ) and find that about 40% of samples in either double or triple regime display distinct velocity discontinuities, i.e., the relative velocities between ^13 CO structures are larger than the internal line widths of ^13 CO structures. Among these 40% samples in the triple regime, 33% exhibit signatures of combinations through the two-body motion, whereas the remaining 7% show features of configurations through the multiple-body motion. The Δ V _LOS distributions for MCs with double and triple ^13 CO structures are similar, as well as their Δ V _LOS / ${\sigma }_{{}^{13}\mathrm{CO},\mathrm{in}}$ distributions. This suggests that relative motions of ^13 CO structures within MCs are random and independent of cloud complexities and scales.https://doi.org/10.3847/1538-3881/ad323aInterstellar mediumInterstellar moleculesMolecular clouds |
| spellingShingle | Lixia Yuan Ji Yang Xuepeng Chen Yang Su Shaobo Zhang Xin Zhou Zhiwei Chen Qing-Zeng Yan Min Fang Fujun Du Yan Sun Hongchi Wang Ye Xu Relative Velocities between 13CO Structures within 12CO Molecular Clouds The Astronomical Journal Interstellar medium Interstellar molecules Molecular clouds |
| title | Relative Velocities between 13CO Structures within 12CO Molecular Clouds |
| title_full | Relative Velocities between 13CO Structures within 12CO Molecular Clouds |
| title_fullStr | Relative Velocities between 13CO Structures within 12CO Molecular Clouds |
| title_full_unstemmed | Relative Velocities between 13CO Structures within 12CO Molecular Clouds |
| title_short | Relative Velocities between 13CO Structures within 12CO Molecular Clouds |
| title_sort | relative velocities between 13co structures within 12co molecular clouds |
| topic | Interstellar medium Interstellar molecules Molecular clouds |
| url | https://doi.org/10.3847/1538-3881/ad323a |
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