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Cloud-cloud collision and star formation in G323.18+0.15

文献类型：期刊论文

作者Ma, Yingxiu3,4; Zhou, Jianjun1,2,4; Esimbek, Jarken1,2,4; Baan, Willem4,5; Li, Dalei1,2,4; He, Yuxin1,2,4; Tang, Xindi1,2,4; Ji, Weiguang1,2,4; Zhou, Dongdong1,2,4; Wu, Gang6
刊名Astronomy & Astrophysics
出版日期2022-07-01
卷号663页码:A97
ISSN号0004-6361
关键词ISM: kinematics and dynamics radio lines: ISM line: formation ISM: clouds ISM: individual objects: G323.18+0.15 galactic plane isolating signatures forming regions complete sample hi-gal filaments cores ii. stability atlasgal Astronomy & Astrophysics
DOI10.1051/0004-6361/202243317
产权排序1
文献子类Article
英文摘要We studied the cloud-cloud collision candidate G323.18+0.15 based on signatures of induced filaments, clumps, and star formation. We used archival molecular spectrum line data from the SEDIGISM (CO)-C-13 (J = 2-1) survey, from the Mopra southern Galactic plane CO survey, and infrared to radio data from the GLIMPSE, MIPS, Hi-GAL, and SGPS surveys. Our new result shows that the G323.18+0.15 complex is 3.55 kpc away from us and consists of three cloud components, G323.18a, G323.18b, and G323.18c. G323.18b shows a perfect U-shape structure, which can be fully complemented by G323.18a, suggesting a collision between G323.18a and the combined G323.18bc filamentary structure. One dense compressed layer (filament) is formed at the bottom of G323.18b, where we detect a greatly increased velocity dispersion. The bridge with an intermediate velocity in a position-velocity diagram appears between G323.18a and G323.18b, which corresponds to the compressed layer. G323.18a plus G323.18b as a whole are probably not gravitationally bound. This indicates that high-mass star formation in the compressed layer may have been caused by an accidental event. The column density in the compressed layer of about 1.36 x 10(22) cm(-2) and most of the dense clumps and high-mass stars are located there. The average surface density of class I and class II young stellar objects (YSOs) inside the G323.18+0.15 complex is much higher than the density in the surroundings. The timescale of the collision between G323.18a and G323.18b is 1.59 Myr. This is longer than the typical lifetime of class I YSOs and is comparable to the lifetime of class II YSOs.
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语种英语
WOS记录号WOS:000827180900003
源URL[http://ir.xao.ac.cn/handle/45760611-7/5140]  
专题恒星形成与演化研究团组
作者单位1.Xinjiang Key Laboratory of Radio Astrophysics, Urumqi 830011, PR China;
2.Key Laboratory of Radio Astronomy, Chinese Academy of Sciences, Urumqi 830011, PR China;
3.University of Chinese Academy of Sciences, Beijing 100049, PR China;
4.XingJiang Astronomical Observatory, Chinese Academy of Sciences,Urumqi 830011, PR China;
5.Netherlands Institute for Radio Astronomy, ASTRON, 7991 PD Dwingeloo, The Netherlands;
6.Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, 53121 Bonn, Germany;
7.Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210008, PR China
推荐引用方式
GB/T 7714		 Ma, Yingxiu,Zhou, Jianjun,Esimbek, Jarken,et al. Cloud-cloud collision and star formation in G323.18+0.15[J]. Astronomy & Astrophysics,2022,663:A97.
APA Ma, Yingxiu.,Zhou, Jianjun.,Esimbek, Jarken.,Baan, Willem.,Li, Dalei.,...&Xu, Ye.(2022).Cloud-cloud collision and star formation in G323.18+0.15.Astronomy & Astrophysics,663,A97.
MLA Ma, Yingxiu,et al."Cloud-cloud collision and star formation in G323.18+0.15".Astronomy & Astrophysics 663(2022):A97.

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