Comparison of NH_(3) and ^(12)CO,^(13)CO,C^(18)O Molecular Lines in the Aquila Rift Cloud Complex  

作　　者：Kadirya Tursun Jarken Esimbek Willem Baan Toktarkhan Komesh Xindi Tang Gang Wu Jianjun Zhou Yuxin He Dalei Li Dongdong Zhou Yingxiu Ma 

机构地区：[1]Xinjiang Astronomical Observatory,Chinese Academy of Sciences,Urumqi 830011,China [2]Key Laboratory of Radio Astronomy,Chinese Academy of Sciences,Urumqi 830011,China [3]Xinjiang Key Laboratory of Radio Astrophysics,Urumqi 830011,China [4]Netherlands Institute for Radio Astronomy,NL-7991PD Dwingeloo,The Netherlands [5]Energetic Cosmos Laboratory,Nazarbayev University,Astana 010000,Kazakhstan [6]Institute of Experimental and Theoretical Physics,Al-Farabi Kazakh National University,Almaty 050040,Kazakhstan

出　　处：《Research in Astronomy and Astrophysics》2024年第9期225-235,共11页天文和天体物理学研究（英文版）

基　　金：supported by the National Key R&D Programs of China(Nos.2023YFA1608002,and 2022YFA1603103);the regional Collaborative Innovation Project of Xinjiang Uyghur Autonomous Region(No.2022E01050);the Tianshan Talent Program of Xinjiang Uyghur Autonomous Region(No.2022TSYCLJ0005);the Tianchi Talent Project of Xinjiang Uyghur Autonomous Region,the Natural Science Foundation of Xinjiang Uyghur Autonomous Region(No.2022D01E06);the Chinese Academy of Sciences(CAS)“Light of West China”Program(Nos.xbzgzdsys-202212,2020-XBQNXZ-017,and 2021-XBQNXZ-028);the National Natural Science Foundation of China(Nos.12173075,11973076,and 12103082);the Xinjiang Key Laboratory of Radio Astrophysics(No.2022D04033);the Chinese Academy of Sciences President's International Fellowship Initiative(Nos.2022VMA0019,and 2023VMA0030);the Science Committee of the Ministry of Science and Higher Education of the Republic of Kazakhstan(No.AP13067768)。

摘　　要：The observations of the Aquila Rift cloud complex at 23.708 and 115.271 GHz made using the Nanshan 26 m radio telescope and the 13.7 m millimeter-wavelength telescope are presented.We find that the CO(1-0)gas distribution is similar to the NH_(3)gas distribution in the Aquila Rift cloud complex.In some diffusion regions characterized by CO,we identified several dense clumps based on the distribution of detected ammonia molecular emission.Through the comparison of spectral line parameters for NH_(3),^(13)CO,and C^(18)O,our study reveals that the line center velocities of the NH_(3),^(13)CO,and C^(18)O lines are comparable and positively correlated,indicating that they originate from the same emission region.No significant correlation was identified for other parameters,including integrated intensity,line widths,main beam brightness temperature,as well as the column densities of NH_(3),^(13)CO,and C^(18)O.The absolute difference in line-center velocities between the^(13)CO and NH_(3)lines is less than both the average line width of NH_(3)and that of^(13)CO.This suggests that there are no significant movements of NH_(3)clumps in relation to their envelopes.The velocity deviation is likely due to turbulent activity within the clumps.

关 键 词：ISM:clouds ISM:molecules stars:formation 

分 类 号：P151[天文地球—天文学]