首页|FAST Observations of Four Comets to Search for the Molecular Line Emissions between 1.0 and 1.5 GHz Frequencies

FAST Observations of Four Comets to Search for the Molecular Line Emissions between 1.0 and 1.5 GHz Frequencies

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We used the Five-hundred-meter Aperture Spherical radio Telescope(FAST)to search for the molecular emissions in the L-band between 1.0 and 1.5 GHz toward four comets,C/2020 F3(NEOWISE),C/2020 R4(ATLAS),C/2021 A1(Leonard),and 67P/Churyumov-Gerasimenko during or after their perihelion passages.Thousands of molecular transition lines fall in this low-frequency range,many attributed to complex organic or prebiotic molecules.We conducted a blind search for the possible molecular lines in this frequency range in those comets and could not identify clear signals of molecular emissions in the data.Although several molecules have been detected at high frequencies of greater than 100 GHz in comets,our results confirm that it is challenging to detect molecular transitions in the L-band frequency ranges.The non-detection of L-band molecular lines in the cometary environment could rule out the possibility of unusually strong lines,which could be caused by the masers or non-LTE effects.Although the line strengths are predicted to be weak,for FAST,using the ultra-wide bandwidth receiver and improving the radio frequency interference environments would enhance the detectability of those molecular transitions at low frequencies in the future.

astrochemistry-ISMmolecules-cometsgeneral-lineidentification

Long-Fei Chen、Chao-Wei Tsai、Jian-Yang Li、Bin Yang、Di Li、Yan Duan、Chih-Hao Hsia、Zhichen Pan、Lei Qian、Donghui Quan、Xue-Jian Jiang、Xiaohu Li、Ruining Zhao、Pei Zuo

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School of Physics and Electronic Science,Guizhou Normal University,Guiyang 550025,China

Guizhou Provincial Key Laboratory of Radio Astronomy and Data Processing,Guiyang 550025,China

Research Center for Astronomical Computing,Zhejiang Laboratory,Hangzhou 311100,China

National Astronomical Observatories,Chinese Academy of Sciences,Beijing 100101,China

Institute for Frontiers in Astronomy and Astrophysics,Beijing Normal University,Beijing 102206,China

Key Laboratory of Radio Astronomy and Technology,Chinese Academy of Sciences,Beijing 100101,China

School of Atmospheric Sciences,Sun Yat-sen University,Zhuhai 519082,China

Núcleo de Astronomía,Facultad de Ingenieríay Ciencias,Universidad Diego Portales,Chile

Department of Astronomy,College of Physics and Electronic Engineering,Qilu Normal University,Jinan 250200,China

Department of Electronic and Optical Engineering,Space Engineering University,Beijing 101416,China

Laboratory for Space Research,Faculty of Science,The University of Hong Kong,Hong Kong(SAR),China

Xinjiang Astronomical Observatory,Chinese Academy of Sciences,Urumqi 830011,China

CAS Key Laboratory of Optical Astronomy,National Astronomical Observatories,Chinese Academy of Sciences,Beijing 100101,China

School of Astronomy and Space Sciences,University of Chinese Academy of Sciences,Beijing 100049,China

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National Natural Science Foundation of China(NSFC)China Postdoctoral Science FoundationFoundation of Education Bureau of Guizhou Province,ChinaInternational Partnership Program of the Chinese Academy of Sciences,programNational Key R&D Program of ChinaNational Key R&D Program of ChinaNSFCNSFCNSFCNSFCNSFCNSFCNSFCCAS"Light of West China"Program and the Youth Innovation Promotion Association of the Chinese Academy of SciencesCAS"Light of West China"Program and the Youth Innovation Promotion Association of the Chinese Academy of SciencesCAS"Light of West China"Program and the Youth Innovation Promotion Association of the Chinese Academy of SciencesNSFC

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2024

10.1088/1674-4527/ad7823

天文和天体物理学研究
中国科学院国家天文台

天文和天体物理学研究

CSTPCD
影响因子：0.406
ISSN：1674-4527
年,卷(期)：2024.24(10)