A SiO J = 5 - 4 Survey Toward Massive Star Formation Regions
Shanghuo Li, Junzhi Wang, Min Fang, Qizhou Zhang, Fei Li, Zhi-Yu, Zhang, Juan Li, Qingfeng Zhu, and Shaoshan Zeng

TL;DR
This survey of 199 massive star-forming regions using SiO J=5-4 line emission reveals diverse shock-related phenomena across different evolutionary stages, with no significant variation in SiO abundance or luminosity among these stages.
Contribution
First large-scale SiO J=5-4 survey across multiple evolutionary stages of massive star formation regions, providing new insights into shock activities and chemical properties.
Findings
SiO emission detected in 57% of sources, with varying detection rates across stages.
Presence of both broad and narrow SiO lines indicating high-velocity and low-velocity shocks.
No significant difference in SiO luminosity or abundance among different evolutionary stages.
Abstract
We performed a survey in the SiO line toward a sample of 199 Galactic massive star-forming regions at different evolutionary stages with the SMT 10 m and CSO 10.4 m telescopes. The sample consists of 44 infrared dark clouds (IRDCs), 86 protostellar candidates, and 69 young \HII\ regions. We detected SiO line emission in 102 sources, with a detection rate of 57\%, 37\%, and 65\% for IRDCs, protostellar candidates, and young \HII\ regions, respectively. We find both broad line with Full Widths at Zero Power (FWZP) 20 \kms and narrow line emissons of SiO in objects at various evolutionary stages, likely associated with high-velocity shocks and low-velocity shocks, respectively. The SiO luminosities do not show apparent differences among various evolutionary stages in our sample. We find no correlation between the SiO abundance and the…
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editorials, notices — miscellaneous — catalogs — surveys
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- 1Kennicutt et al. (2006) Kennicutt, R. C., Jr., Vishniac, E., & Sneden, C. 2006, Ap J, 652, 847
- 2Kurtz et al. (2000) Kurtz, M. J., Eichhorn, G., Accomazzi, A., et al. 2000, A&AS, 143, 41
- 3Vishniac (2012) Vishniac, E. T. 2012, American Astronomical Society Meeting Abstracts #219, 219, 204.04
