Giant Molecular Clouds in RCW 106 (G333): Galactic Mini-starbursts and Massive Star Formation Induced by Supersonic Cloud-Cloud Collisions
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| Main Authors: | , , , , , , , , , , , , , , , |
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| Format: | Preprint |
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2025
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| author | Kohno, Mikito Yamada, Rin I. Tachihara, Kengo Fujita, Shinji Enokiya, Rei Tokuda, Kazuki Habe, Asao Sano, Hidetoshi Hayakawa, Takahiro Demachi, Fumika Ito, Takuto Tsuge, Kisetsu Nishimura, Atsushi Kobayashi, Masato I. N. Yamamoto, Hiroaki Fukui, Yasuo |
| author_facet | Kohno, Mikito Yamada, Rin I. Tachihara, Kengo Fujita, Shinji Enokiya, Rei Tokuda, Kazuki Habe, Asao Sano, Hidetoshi Hayakawa, Takahiro Demachi, Fumika Ito, Takuto Tsuge, Kisetsu Nishimura, Atsushi Kobayashi, Masato I. N. Yamamoto, Hiroaki Fukui, Yasuo |
| contents | To reveal the origin of the mini-starbursts in the Milky Way, we carried out large-scale CO observations toward the RCW 106 giant molecular cloud (GMC) complex using the NANTEN2 4-m radio telescope operated by Nagoya University. We also analyzed the Mopra Southern Galactic plane CO survey and Herschel infrared continuum archival data. The RCW 106 GMC complex contains the radial velocity components of $-68$ km s$^{-1}$ and $-50$ km s$^{-1}$ reported by Nguyen et al. (2015). Focusing on the RCW 106 East and West region with the massive star formation having the bright infrared dust emission, we found that these regions have three different velocity components with $\sim 10$ km s$^{-1}$ differences. The two out of three velocity components show morphological correspondence with the infrared cold dust emission and connect with the bridge feature on a position-velocity diagram. Therefore, two molecular clouds (MCs) with $\sim 10$ km s$^{-1}$ differences are likely to be physically associated with massive star-forming regions in the GMC complex. Based on these observational results, we argue that mini-starbursts and massive star/cluster formation in the RCW 106 GMC complex are induced by supersonic cloud-cloud collisions in an agglomerate of molecular gas on the Scutum-Centaurus arm. |
| format | Preprint |
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arxiv_https___arxiv_org_abs_2501_14575 |
| institution | arXiv |
| publishDate | 2025 |
| record_format | arxiv |
| spellingShingle | Giant Molecular Clouds in RCW 106 (G333): Galactic Mini-starbursts and Massive Star Formation Induced by Supersonic Cloud-Cloud Collisions Kohno, Mikito Yamada, Rin I. Tachihara, Kengo Fujita, Shinji Enokiya, Rei Tokuda, Kazuki Habe, Asao Sano, Hidetoshi Hayakawa, Takahiro Demachi, Fumika Ito, Takuto Tsuge, Kisetsu Nishimura, Atsushi Kobayashi, Masato I. N. Yamamoto, Hiroaki Fukui, Yasuo Astrophysics of Galaxies To reveal the origin of the mini-starbursts in the Milky Way, we carried out large-scale CO observations toward the RCW 106 giant molecular cloud (GMC) complex using the NANTEN2 4-m radio telescope operated by Nagoya University. We also analyzed the Mopra Southern Galactic plane CO survey and Herschel infrared continuum archival data. The RCW 106 GMC complex contains the radial velocity components of $-68$ km s$^{-1}$ and $-50$ km s$^{-1}$ reported by Nguyen et al. (2015). Focusing on the RCW 106 East and West region with the massive star formation having the bright infrared dust emission, we found that these regions have three different velocity components with $\sim 10$ km s$^{-1}$ differences. The two out of three velocity components show morphological correspondence with the infrared cold dust emission and connect with the bridge feature on a position-velocity diagram. Therefore, two molecular clouds (MCs) with $\sim 10$ km s$^{-1}$ differences are likely to be physically associated with massive star-forming regions in the GMC complex. Based on these observational results, we argue that mini-starbursts and massive star/cluster formation in the RCW 106 GMC complex are induced by supersonic cloud-cloud collisions in an agglomerate of molecular gas on the Scutum-Centaurus arm. |
| title | Giant Molecular Clouds in RCW 106 (G333): Galactic Mini-starbursts and Massive Star Formation Induced by Supersonic Cloud-Cloud Collisions |
| topic | Astrophysics of Galaxies |
| url | https://arxiv.org/abs/2501.14575 |