ATOMS: ALMA Three-millimeter Observations of Massive Star-forming regions -- XIX. The origin of SiO emission
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| Main Authors: | , , , , , , , , , , , , , , , , , , , , , , , , , |
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| Format: | Preprint |
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2024
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| author | Liu, Rong Liu, Tie Jiménez-Serra, Izaskun Li, Jin-Zeng Martín-Pintado, Jesús Liu, Xunchuan Lee, Chang Won Sanhueza, Patricio Chibueze, James O. Rivilla, Víctor M. Juvela, Mika Colzi, Laura Bronfman, Leonardo Liu, Hong-Li Sanz-Novo, Miguel López-Gallifa, Álvaro Li, Shanghuo Megías, Andrés Andrés, David San Garay, Guido Hwang, Jihye Zhou, Jianwen Xu, Fengwei Martínez-Henares, Antonio Saha, Anindya Nazeer, Hafiz |
| author_facet | Liu, Rong Liu, Tie Jiménez-Serra, Izaskun Li, Jin-Zeng Martín-Pintado, Jesús Liu, Xunchuan Lee, Chang Won Sanhueza, Patricio Chibueze, James O. Rivilla, Víctor M. Juvela, Mika Colzi, Laura Bronfman, Leonardo Liu, Hong-Li Sanz-Novo, Miguel López-Gallifa, Álvaro Li, Shanghuo Megías, Andrés Andrés, David San Garay, Guido Hwang, Jihye Zhou, Jianwen Xu, Fengwei Martínez-Henares, Antonio Saha, Anindya Nazeer, Hafiz |
| contents | The production of silicon monoxide (SiO) can be considered as a fingerprint of shock interaction. In this work, we use high-sensitivity observations of the SiO (2-1) and H$^{13}$CO$^{+}$ (1-0) emission to investigate the broad and narrow SiO emission toward 146 massive star-forming regions in the ATOMS survey. We detected SiO emission in 136 regions and distinguished broad and narrow components across the extension of 118 sources (including 58 UC $H_{II}$ regions) with an average angular resolution of 2.5$^{\prime}$$^{\prime}$. The derived SiO luminosity ($L_{SiO}$) across the whole sample shows that the majority of $L_{SiO}$ (above 66$\%$) can be attributed to broad SiO, indicating its association with strong outflows. The comparison of the ALMA SiO images with the filamentary skeletons identified from H$^{13}$CO$^{+}$ and in the infrared data (at 4.5, 8, and 24 $mu$m), further confirms that most SiO emission originates from outflows. However, note that for nine sources in our sample, the observed SiO emission may be generated by expanding UC $H_{II}$ regions. There is a moderate positive correlation between the bolometric luminosity ($L_{bol}$) and $L_{SiO}$ for both components (narrow and broad). The UC $H_{II}$ sources show a weaker positive correlation between $L_{bol}$ and $L_{SiO}$ and higher $L_{SiO}$ compared to the sources without UC $H_{II}$ regions. These results imply that the SiO emission from UC $H_{II}$ sources might be affected by UV-photochemistry induced by UC $H_{II}$ regions. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2411_19489 |
| institution | arXiv |
| publishDate | 2024 |
| record_format | arxiv |
| spellingShingle | ATOMS: ALMA Three-millimeter Observations of Massive Star-forming regions -- XIX. The origin of SiO emission Liu, Rong Liu, Tie Jiménez-Serra, Izaskun Li, Jin-Zeng Martín-Pintado, Jesús Liu, Xunchuan Lee, Chang Won Sanhueza, Patricio Chibueze, James O. Rivilla, Víctor M. Juvela, Mika Colzi, Laura Bronfman, Leonardo Liu, Hong-Li Sanz-Novo, Miguel López-Gallifa, Álvaro Li, Shanghuo Megías, Andrés Andrés, David San Garay, Guido Hwang, Jihye Zhou, Jianwen Xu, Fengwei Martínez-Henares, Antonio Saha, Anindya Nazeer, Hafiz Astrophysics of Galaxies The production of silicon monoxide (SiO) can be considered as a fingerprint of shock interaction. In this work, we use high-sensitivity observations of the SiO (2-1) and H$^{13}$CO$^{+}$ (1-0) emission to investigate the broad and narrow SiO emission toward 146 massive star-forming regions in the ATOMS survey. We detected SiO emission in 136 regions and distinguished broad and narrow components across the extension of 118 sources (including 58 UC $H_{II}$ regions) with an average angular resolution of 2.5$^{\prime}$$^{\prime}$. The derived SiO luminosity ($L_{SiO}$) across the whole sample shows that the majority of $L_{SiO}$ (above 66$\%$) can be attributed to broad SiO, indicating its association with strong outflows. The comparison of the ALMA SiO images with the filamentary skeletons identified from H$^{13}$CO$^{+}$ and in the infrared data (at 4.5, 8, and 24 $mu$m), further confirms that most SiO emission originates from outflows. However, note that for nine sources in our sample, the observed SiO emission may be generated by expanding UC $H_{II}$ regions. There is a moderate positive correlation between the bolometric luminosity ($L_{bol}$) and $L_{SiO}$ for both components (narrow and broad). The UC $H_{II}$ sources show a weaker positive correlation between $L_{bol}$ and $L_{SiO}$ and higher $L_{SiO}$ compared to the sources without UC $H_{II}$ regions. These results imply that the SiO emission from UC $H_{II}$ sources might be affected by UV-photochemistry induced by UC $H_{II}$ regions. |
| title | ATOMS: ALMA Three-millimeter Observations of Massive Star-forming regions -- XIX. The origin of SiO emission |
| topic | Astrophysics of Galaxies |
| url | https://arxiv.org/abs/2411.19489 |