Planck Galactic Cold Clumps at High Galactic Latitude—a Study with CO Lines

• Published in: The Astrophysical journal 2021-10, Vol.920 (2), p.103
• Main Authors: Xu, Fengwei, Wu, Yuefang, Liu, Tie, Liu, Xunchuan, Zhang, Chao, Esimbek, Jarken, Qin, Sheng-Li, Li, Di, Wang, Ke, Yuan, Jinghua, Meng, Fanyi, Zhang, Tianwei, Eden, David, Tatematsu, K., Evans, Neal J., Goldsmith, Paul. F., Zhang, Qizhou, Henkel, C., Yi, Hee-Weon, Lee, Jeong-Eun, Saajasto, Mika, Kim, Gwanjeong, Juvela, Mika, Sahu, Dipen, Hsu, Shih-Ying, Liu, Sheng-Yuan, Dutta, Somnath, Lee, Chin-Fei, Zhang, Chuan-Peng, Xu, Ye, Ju, Binggang
• Format: Article
• Language: English
• Subjects: Astrophysics; Clumps; Cores; Dark interstellar clouds; Emission; Galactic disk; Interstellar matter; Interstellar medium; Interstellar molecules; Latitude; Mountains; Solar neighborhood; Star & galaxy formation; Star formation; Turbulence; Velocity
• ISSN: 0004-637X; 1538-4357
• DOI: 10.3847/1538-4357/ac1686

Gas at high Galactic latitude is a relatively little noticed component of the interstellar medium. In an effort to address this, 41 Planck Galactic Cold Clumps at high Galactic latitude (HGal; ∣ b ∣ > 25°) were observed in 12 CO, 13 CO, and C 18 O J = 1−0 lines, using the Purple Mountain Observatory 13.7 m telescope. 12 CO (1−0) and 13 CO (1−0) emission was detected in all clumps, while C 18 O (1−0) emission was only seen in 16 clumps. The highest and average latitudes are 71.°4 and 37.°8, respectively. Fifty-one velocity components were obtained, and then each was identified as a single clump. Thirty-three clumps were further mapped at 1′ resolution, and 54 dense cores were extracted. Among dense cores, the average excitation temperature T ex of 12 CO is 10.3 K. The average line widths of thermal and nonthermal velocity dispersions are 0.19 and 0.46 km s −1 , respectively, suggesting that these cores are dominated by turbulence. Distances of the HGal clumps given by Gaia dust reddening are about 120–360 pc. The ratio of X 13 / X 18 is significantly higher than that in the solar neighborhood, implying that HGal gas has a different star formation history compared to the gas in the Galactic disk. HGal cores with sizes from 0.01 to 0.1 pc show no notable Larson’s relation, and the turbulence remains supersonic down to a scale of slightly below 0.1 pc. None of the HGal cores that bear masses from 0.01 to 1 M ⊙ are gravitationally bound, and all appear to be confined by outer pressure.