ACA CO(J=2-1) Mapping of the Nearest Spiral Galaxy M33. II. Exploring the Evolution of Giant Molecular Clouds
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| Main Authors: | , , , , , , , , , , , , , , |
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| Format: | Preprint |
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2024
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| _version_ | 1866929478463127552 |
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| author | Konishi, Ayu Muraoka, Kazuyuki Tokuda, Kazuki Fujita, Shinji Fukui, Yasuo Yamada, Rin I. Demachi, Fumika Tachihara, Kengo Kobayashi, Masato I. N. Kuno, Nario Tsuge, Kisetsu Sano, Hidetoshi Miura, Rie E. Kawamura, Akiko Onishi, Toshikazu |
| author_facet | Konishi, Ayu Muraoka, Kazuyuki Tokuda, Kazuki Fujita, Shinji Fukui, Yasuo Yamada, Rin I. Demachi, Fumika Tachihara, Kengo Kobayashi, Masato I. N. Kuno, Nario Tsuge, Kisetsu Sano, Hidetoshi Miura, Rie E. Kawamura, Akiko Onishi, Toshikazu |
| contents | The evolution of giant molecular clouds (GMCs), the main sites of high-mass star formation, is an essential process to unravel the galaxy evolution. Using a GMC catalogue of M33 from ALMA-ACA survey, we classified 848 GMCs into three types based on the association with HII regions and their H$α$ luminosities $\textit{L}$(H$α$): Type I is associated with no HII regions; Type II with HII regions of $\textit{L}$(H$α$) $<$ 10$^{37.5}$ erg s$^{-1}$; and Type III with HII regions of $\textit{L}$(H$α$) $\geqq$ 10$^{37.5}$ erg s$^{-1}$. These criteria yield 224 Type I GMCs, 473 Type II GMCs, and 151 Type III GMCs. GMCs show changes in their physical properties according to the types; mass, radius, velocity dispersion, and $^{13}$CO detection rate of GMCs systematically increase from Type I to Type III, and additionally, Type III GMCs are closest to virial equilibrium. Type III GMCs show the highest spatial correlation with clusters younger than 10 Myr, Type II GMCs moderate correlation, and Type I GMCs are almost uncorrelated. We interpret that these types indicate an evolutionary sequence from Type I to Type II, and then to Type III with timescales of 4 Myr, 13 Myr, and 5 Myr, respectively, indicating the GMC lifetime of 22 Myr by assuming that Type II GMC has the same timescale as the Large Magellanic Cloud. The evolved GMCs concentrate on the spiral arms, while the younger GMCs are apart from the arm both to the leading and trailing sides. This indicated that GMCs collide with each other by the spiral potential, leading to the compression of GMCs and the triggering of high-mass star formation, which may support the dynamic spiral model. Overall, we suggest that the GMC evolution concept helps illuminate the galaxy evolution, including the spiral arm formation. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2407_17018 |
| institution | arXiv |
| publishDate | 2024 |
| record_format | arxiv |
| spellingShingle | ACA CO(J=2-1) Mapping of the Nearest Spiral Galaxy M33. II. Exploring the Evolution of Giant Molecular Clouds Konishi, Ayu Muraoka, Kazuyuki Tokuda, Kazuki Fujita, Shinji Fukui, Yasuo Yamada, Rin I. Demachi, Fumika Tachihara, Kengo Kobayashi, Masato I. N. Kuno, Nario Tsuge, Kisetsu Sano, Hidetoshi Miura, Rie E. Kawamura, Akiko Onishi, Toshikazu Astrophysics of Galaxies The evolution of giant molecular clouds (GMCs), the main sites of high-mass star formation, is an essential process to unravel the galaxy evolution. Using a GMC catalogue of M33 from ALMA-ACA survey, we classified 848 GMCs into three types based on the association with HII regions and their H$α$ luminosities $\textit{L}$(H$α$): Type I is associated with no HII regions; Type II with HII regions of $\textit{L}$(H$α$) $<$ 10$^{37.5}$ erg s$^{-1}$; and Type III with HII regions of $\textit{L}$(H$α$) $\geqq$ 10$^{37.5}$ erg s$^{-1}$. These criteria yield 224 Type I GMCs, 473 Type II GMCs, and 151 Type III GMCs. GMCs show changes in their physical properties according to the types; mass, radius, velocity dispersion, and $^{13}$CO detection rate of GMCs systematically increase from Type I to Type III, and additionally, Type III GMCs are closest to virial equilibrium. Type III GMCs show the highest spatial correlation with clusters younger than 10 Myr, Type II GMCs moderate correlation, and Type I GMCs are almost uncorrelated. We interpret that these types indicate an evolutionary sequence from Type I to Type II, and then to Type III with timescales of 4 Myr, 13 Myr, and 5 Myr, respectively, indicating the GMC lifetime of 22 Myr by assuming that Type II GMC has the same timescale as the Large Magellanic Cloud. The evolved GMCs concentrate on the spiral arms, while the younger GMCs are apart from the arm both to the leading and trailing sides. This indicated that GMCs collide with each other by the spiral potential, leading to the compression of GMCs and the triggering of high-mass star formation, which may support the dynamic spiral model. Overall, we suggest that the GMC evolution concept helps illuminate the galaxy evolution, including the spiral arm formation. |
| title | ACA CO(J=2-1) Mapping of the Nearest Spiral Galaxy M33. II. Exploring the Evolution of Giant Molecular Clouds |
| topic | Astrophysics of Galaxies |
| url | https://arxiv.org/abs/2407.17018 |