Ammonia observations towards the Aquila Rift cloud complex

doi:10.1051/0004-6361/202037659

	Ammonia observations towards the Aquila Rift cloud complex
	Tursun, Kadirya 3,4; Esimbek, Jarken 3,5; Henkel, Christian 1,3,6; Tang, Xindi 1,3,5; Wu, Gang 3,5; Li, Dalei 3,5; Zhou, Jianjun 3,5; He, Yuxin 3,5; Komesh, Toktarkhan 2,3,4; Sailanbek, Serikbek 2,3,4
刊名	ASTRONOMY & ASTROPHYSICS
	2020-11-20
卷号	643 页码:178
关键词	surveys radio lines: ISM ISM: molecules ISM: kinematics and dynamics stars: formation
ISSN号	0004-6361
DOI	10.1051/0004-6361/202037659
产权排序	1
英文摘要	We surveyed the Aquila Rift complex including the Serpens South and W 40 regions in the NH3 (1,1) and (2,2) transitions making use of the Nanshan 26-m telescope. Our observations cover an area of similar to 1.5 degrees x 2.2 degrees (11.4 pc x 16.7 pc). The kinetic temperatures of the dense gas in the Aquila Rift complex obtained from NH3 (2,2)/(1,1) ratios range from 8.9 to 35.0 K with an average of 15.3 +/- 6.1 K (errors are standard deviations of the mean). Low gas temperatures are associated with Serpens South ranging from 8.9 to 16.8 K with an average of 12.3 +/- 1.7 K, while dense gas in the W 40 region shows higher temperatures ranging from 17.7 to 35.0 K with an average of 25.1 +/- 4.9 K. A comparison of kinetic temperatures derived from para-NH3 (2,2)/(1,1) against HiGal dust temperatures indicates that the gas and dust temperatures are in agreement in the low-mass-star formation region of Serpens South. In the high-mass-star formation region W 40, the measured gas kinetic temperatures are higher than those of the dust. The turbulent component of the velocity dispersion of NH3 (1,1) is found to be positively correlated with the gas kinetic temperature, which indicates that the dense gas may be heated by dissipation of turbulent energy. For the fractional total-NH3 (para+ortho) abundance obtained by a comparison with Herschel infrared continuum data representing dust emission, we find values from 0.1 x10(-8) to 2.1 x10(-7) with an average of 6.9 (+/- 4.5) x 10(-8). Serpens South also shows a fractional total-NH3 (para+ortho) abundance ranging from 0.2 x10(-8) to 2.1 x10(-7) with an average of 8.6 (+/- 3.8) x 10(-8). In W 40, values are lower, between 0.1 and 4.3 x10(-8) with an average of 1.6 (+/- 1.4) x 10(-8). Weak velocity gradients demonstrate that the rotational energy is a negligible fraction of the gravitational energy. In W 40, gas and dust temperatures are not strongly dependent on the projected distance to the recently formed massive stars. Overall, the morphology of the mapped region is ring-like, with strong emission at lower and weak emission at higher Galactic longitudes. However, the presence of a physical connection between the two parts remains questionable.
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资助项目	National Natural Science foundation of China[11433008] ; National Natural Science foundation of China[11903070] ; National Natural Science foundation of China[11603063] ; National Natural Science foundation of China[11703074] ; National Natural Science foundation of China[11703073] ; National Natural Science foundation of China[11973076] ; Heaven Lake Hundred-Talent Program of Xinjiang Uygur Autonomous Region of China ; CAS Light of West China Program[2018-XBQNXZ-B-024] ; CAS Light of West China Program[2016-QNXZ-B-23] ; CAS Light of West China Program[2016-QNXZ-B-22] ; Chinese Academy of Sciences[2021VMA0009]
WOS关键词	STAR-FORMING REGIONS ; DENSE CORES ; DARK CLOUDS ; PHYSICAL CONDITIONS ; INTERNAL STRUCTURE ; THERMAL BALANCE ; IRAS SOURCES ; NH3 ; ORION ; CLUSTER
WOS研究方向	Astronomy & Astrophysics
语种	英语
出版者	EDP SCIENCES S A
WOS记录号	WOS:000595643700003
资助机构	National Natural Science foundation of China ; Heaven Lake Hundred-Talent Program of Xinjiang Uygur Autonomous Region of China ; CAS Light of West China Program ; Chinese Academy of Sciences
内容类型	期刊论文
源URL	[http://ir.xao.ac.cn/handle/45760611-7/3734]
专题	新疆天文台_射电天文研究室
通讯作者	Esimbek, Jarken; Henkel, Christian; Tang, Xindi
作者单位	1.Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany 2.Al Farabi Kazakh Natl Univ, Fac Phys & Technol, Dept Solid State Phys & Nonlinear Phys, Alma Ata 050040, Kazakhstan 3.Chinese Acad Sci, Xinjiang Astron Observ, Urumqi 830011, Peoples R China 4.Univ Chinese Acad Sci, Beijing 100080, Peoples R China 5.Chinese Acad Sci, Key Lab Radio Astron, Urumqi 830011, Peoples R China 6.King Abdulaziz Univ, Astron Dept, POB 80203, Jeddah 21589, Saudi Arabia
推荐引用方式 GB/T 7714	Tursun, Kadirya,Esimbek, Jarken,Henkel, Christian,et al. Ammonia observations towards the Aquila Rift cloud complex[J]. ASTRONOMY & ASTROPHYSICS,2020,643:178.
APA	Tursun, Kadirya.,Esimbek, Jarken.,Henkel, Christian.,Tang, Xindi.,Wu, Gang.,...&Sailanbek, Serikbek.(2020).Ammonia observations towards the Aquila Rift cloud complex.ASTRONOMY & ASTROPHYSICS,643,178.
MLA	Tursun, Kadirya,et al."Ammonia observations towards the Aquila Rift cloud complex".ASTRONOMY & ASTROPHYSICS 643(2020):178.