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Ammonia observations towards the Aquila Rift cloud complex
Tursun, Kadirya1,2; Esimbek, Jarken1,3; Henkel, Christian1,4,5; Tang, Xindi1,3,4; Wu, Gang1,3; Li, Dalei1,3; Zhou, Jianjun1,3; He, Yuxin1,3; Komesh, Toktarkhan1,2,6; Sailanbek, Serikbek1,2,6
2020-11-20
Source PublicationASTRONOMY & ASTROPHYSICS
ISSN0004-6361
Volume643Pages:178
Contribution Rank1
AbstractWe 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.
Keywordsurveys radio lines: ISM ISM: molecules ISM: kinematics and dynamics stars: formation
DOI10.1051/0004-6361/202037659
URL查看原文
Indexed BySCI
Language英语
WOS KeywordSTAR-FORMING REGIONS ; DENSE CORES ; DARK CLOUDS ; PHYSICAL CONDITIONS ; INTERNAL STRUCTURE ; THERMAL BALANCE ; IRAS SOURCES ; NH3 ; ORION ; CLUSTER
Funding ProjectNational 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 Research AreaAstronomy & Astrophysics
WOS SubjectAstronomy & Astrophysics
WOS IDWOS:000595643700003
PublisherEDP SCIENCES S A
Funding OrganizationNational 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
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Document Type期刊论文
Identifierhttp://ir.xao.ac.cn/handle/45760611-7/3735
Collection射电天文研究室_恒星形成与演化研究团组
射电天文研究室
Corresponding AuthorEsimbek, Jarken; Henkel, Christian; Tang, Xindi
Affiliation1.Chinese Acad Sci, Xinjiang Astron Observ, Urumqi 830011, Peoples R China
2.Univ Chinese Acad Sci, Beijing 100080, Peoples R China
3.Chinese Acad Sci, Key Lab Radio Astron, Urumqi 830011, Peoples R China
4.Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany
5.King Abdulaziz Univ, Astron Dept, POB 80203, Jeddah 21589, Saudi Arabia
6.Al Farabi Kazakh Natl Univ, Fac Phys & Technol, Dept Solid State Phys & Nonlinear Phys, Alma Ata 050040, Kazakhstan
First Author AffilicationXinjiang Astronomical Observatory, Chinese Academy of Sciences
Corresponding Author AffilicationXinjiang Astronomical Observatory, Chinese Academy of Sciences
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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.
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