Gas emission and dynamics in the infrared dark cloud G31.23＋0.05

We performed a multiwavelength study towards the infrared dark cloud （IRDC） G31.23＋0.05 with new CO observations from Purple Mountain Observatory and archival data （the GLIMPSE, MIPSGAL, HERSCHEL, ATLASGAL, BGPS and NVSS surveys）. From these observations, we iden- tified three IRDCs with systemic ve...

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Published in:Research in astronomy and astrophysics 2017-03, Vol.17 (4), p.35-48
Main Authors: Liu, Xiao-Lan, Wang, Jun-Jie, Xu, Jin-Long, Zhang, Chuan-Peng
Format: Article
Language:English
Subjects:
Clouds
Dust
HII区
Infrared
ISM: HII regions
ISM: individual (IRDC G31.23+0.05)
ISM: kinematics and dynamics
ISM: molecules
Masers
Massive stars
Molecular structure
Mountains
OH脉泽
Stars
stars: formation
大质量恒星
气体排放
粉尘排放
紫金山天文台
红外源
速度信息
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cited_by cdi_FETCH-LOGICAL-c514t-8573c25763eed66d52f117e505e57ac2ecad41af1f2dbec11e420104f206432a3
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creator Liu, Xiao-Lan
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description We performed a multiwavelength study towards the infrared dark cloud （IRDC） G31.23＋0.05 with new CO observations from Purple Mountain Observatory and archival data （the GLIMPSE, MIPSGAL, HERSCHEL, ATLASGAL, BGPS and NVSS surveys）. From these observations, we iden- tified three IRDCs with systemic velocities of 108.36 ± 0.06 （cloud A）, 104.22 ± 0.11 （cloud B） and 75.73 ± 0.07 km s-1 （cloud C） in the line of sight towards IRDC G31.23. Analyses of the molecular and dust emission suggest that cloud A is a filamentary structure containing a young stellar object; clouds B and C both include a starless core. Clouds A and B are gravitationally bound and have a chance to form stars. In addition, the velocity information and the position-velocity diagram suggest that clouds A and B are adjacent in space and provide a clue hinting at a possible cloud-cloud collision. Additionally, the distribution of dust temperature shows a temperature bubble. The compact core in cloud A is associated with an UCHII region, an IRAS source, H20 masers, CH3OH masers and OH masers, suggesting that massive star formation is active there. We estimate the age of the HII region to be （0.03-0.09）Myr, indicating that the star inside is young.
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From these observations, we iden- tified three IRDCs with systemic velocities of 108.36 ± 0.06 （cloud A）, 104.22 ± 0.11 （cloud B） and 75.73 ± 0.07 km s-1 （cloud C） in the line of sight towards IRDC G31.23. Analyses of the molecular and dust emission suggest that cloud A is a filamentary structure containing a young stellar object; clouds B and C both include a starless core. Clouds A and B are gravitationally bound and have a chance to form stars. In addition, the velocity information and the position-velocity diagram suggest that clouds A and B are adjacent in space and provide a clue hinting at a possible cloud-cloud collision. Additionally, the distribution of dust temperature shows a temperature bubble. The compact core in cloud A is associated with an UCHII region, an IRAS source, H20 masers, CH3OH masers and OH masers, suggesting that massive star formation is active there. 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From these observations, we iden- tified three IRDCs with systemic velocities of 108.36 ± 0.06 （cloud A）, 104.22 ± 0.11 （cloud B） and 75.73 ± 0.07 km s-1 （cloud C） in the line of sight towards IRDC G31.23. Analyses of the molecular and dust emission suggest that cloud A is a filamentary structure containing a young stellar object; clouds B and C both include a starless core. Clouds A and B are gravitationally bound and have a chance to form stars. In addition, the velocity information and the position-velocity diagram suggest that clouds A and B are adjacent in space and provide a clue hinting at a possible cloud-cloud collision. Additionally, the distribution of dust temperature shows a temperature bubble. The compact core in cloud A is associated with an UCHII region, an IRAS source, H20 masers, CH3OH masers and OH masers, suggesting that massive star formation is active there. 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2397-6209
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source Institute of Physics
subjects Clouds
Dust
HII区
Infrared
ISM: HII regions
ISM: individual (IRDC G31.23+0.05)
ISM: kinematics and dynamics
ISM: molecules
Masers
Massive stars
Molecular structure
Mountains
OH脉泽
Stars
stars: formation
大质量恒星
气体排放
粉尘排放
紫金山天文台
红外源
速度信息
title Gas emission and dynamics in the infrared dark cloud G31.23＋0.05
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