中国物理B ›› 2023, Vol. 32 ›› Issue (2): 29801-029801.doi: 10.1088/1674-1056/aca7ed

• • 上一篇    

Atlas of dynamic spectra of fast radio burst FRB 20201124A

Bo-Jun Wang(王铂钧)1,2,3, Heng Xu(胥恒)2, Jin-Chen Jiang(姜金辰)2, Jiang-Wei Xu(徐江伟)1,2,3, Jia-Rui Niu(牛佳瑞)2,4, Ping Chen(陈平)1,3,5, Ke-Jia Lee(李柯伽)1,2,†, Bing Zhang(张冰)6,7,‡, Wei-Wei Zhu(朱炜玮)2,§, Su-Bo Dong(东苏勃)1, Chun-Feng Zhang(张春风)2, Hai Fu(傅海)8, De-Jiang Zhou(周德江)2,4, Yong-Kun Zhang(张永坤)2,4, Pei Wang(王培)2, Yi Feng(冯毅)2,9, Ye Li(李晔)10, Dong-Zi Li(李冬子)11, Wen-Bin Lu(鲁文宾)12, Yuan-Pei Yang(杨元培)13, R. N. Caballero1,3, Ce Cai(蔡策)14, Mao-Zheng Chen(陈卯蒸)15, Zi-Gao Dai(戴子高)16, A. Esamdin(艾力·伊沙木丁)15, Heng-Qian Gan(甘恒谦)2, Jin-Lin Han(韩金林)2, Long-Fei Hao(郝龙飞)17, Yu-Xiang Huang(黄玉祥)17, Peng Jiang(姜鹏)2, Cheng-Kui Li(李承奎)14, Di Li(李菂)2,18, Hui Li(李辉)2, Xin-Qiao Li(李新乔)14, Zhi-Xuan Li(李志玄)17, Zhi-Yong Liu(刘志勇)15, Rui Luo(罗睿)19, Yun-Peng Men(门云鹏)20, Chen-Hui Niu(牛晨辉)2, Wen-Xi Peng(彭文溪)14, Lei Qian(钱磊)2, Li-Ming Song(宋黎明)14, Jing-Hai Sun(孙京海)2, Fa-Yin Wang(王发印)21, Min Wang(汪敏)17, Na Wang(王娜)15, Wei-Yang Wang(王维扬)3, Xue-Feng Wu(吴雪峰)10, Shuo Xiao(肖硕)14, Shao-Lin Xiong(熊少林)14, Yong-Hua Xu(徐永华)17, Ren-Xin Xu(徐仁新)1,3,22, Jun Yang(杨俊)21, Xuan Yang(杨轩)10, Rui Yao(姚蕊)2, Qi-Bin Yi(易祁彬)14, You-Ling Yue(岳友岭)2, Dong-Jun Yu(于东俊)2, Wen-Fei Yu(余文飞)23, Jian-Ping Yuan(袁建平)15, Bin-Bin Zhang(张彬彬)21,24, Song-Bo Zhang(张松波)10, Shuang-Nan Zhang(张双南)14, Yi Zhao(赵一)14, Wei-Kang Zheng(郑伟康)12, Yan Zhu(朱岩)2, and Jin-Hang Zou(邹金航)21,25   

  1. 1 Kavli Institute for Astronomy and Astrophysics, Peking University, Beijing 100871, China;
    2 National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100101, China;
    3 Department of Astronomy, Peking University, Beijing 100871, China;
    4 University of Chinese Academy of Sciences, Chinese Academy of Sciences, Beijing 100049, China;
    5 Department of Particle Physics and Astrophysics, Weizmann Institute of Science, Rehovot 76100, Israel;
    6 Nevada Center for Astrophysics, University of Nevada, Las Vegas, NV 89154, USA;
    7 Department of Physics and Astronomy, University of Nevada, Las Vegas, NV 89154, USA;
    8 Department of Physics & Astronomy, University of Iowa, Iowa City, IA 52242, USA;
    9 Zhejiang Laboratory, Hangzhou, Zhejiang 311121, China;
    10 Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210008, China;
    11 TAPIR, Walter Burke Institute for Theoretical Physics, Mail Code 350-17, Caltech, Pasadena, CA 91125, USA;
    12 Department of Astronomy, University of California at Berkeley, Berkeley, CA 94720, USA;
    13 South-Western Institute For Astronomy Research, Yunnan University, Yunnan 650504, China;
    14 Key Laboratory of Particle Astrophysics, Institute of High Energy Physics, Chinese Academy of Sciences, Beijing 100049, China;
    15 Xinjiang Astronomical Observatory, Chinese Academy of Sciences, Urumqi 830011, China;
    16 University of Science and Technology of China, Anhui 230026, China;
    17 Yunnan Observatories, Chinese Academy of Sciences, Kunming 650216, China;
    18 Guizhou Normal University, Guiyang 550001, China;
    19 CSIRO Space and Astronomy, Epping, NSW 1710, Australia;
    20 Max-Planck institut für Radioastronomie, Auf Dem Hügel, Bonn, 53121, Germany;
    21 School of Astronomy and Space Science, Nanjing University, Nanjing 210093, China;
    22 State Key Laboratory of Nuclear Physics and Technology, School of Physics, Peking University, Beijing 100871, China;
    23 Shanghai Astronomical Observatory, Chinese Academy of Sciences, Shanghai 200030, China;
    24 Key Laboratory of Modern Astronomy and Astrophysics (Nanjing University), Ministry of Education, Nanjing 210093, China;
    25 College of Physics, Hebei Normal University, Shijiazhuang 050024, China
  • 收稿日期:2022-10-04 修回日期:2022-11-16 接受日期:2022-12-02 出版日期:2023-01-10 发布日期:2023-01-31
  • 通讯作者: Ke-Jia Lee, Bing Zhang, Wei-Wei Zhu E-mail:kjlee@pku.edu.cn;bing.zhang@unlv.edu;zhuww@nao.cas.cn
  • 基金资助:
    This work made use of data from the FAST. FAST is a Chinese national megascience facility, built and operated by the National Astronomical Observatories, Chinese Academy of Sciences. We acknowledge the use of public data from the Fermi Science Support Center (FSSC). This work is supported by the National SKA Program of China (Grant Nos. 2020SKA0120100 and 2020SKA0120200), the National Natural Science Foundation of China (Grant Nos. 12041304, 11873067, 11988101, 12041303, 11725313, 11725314, 11833003, 12003028, 12041306, 12103089, U2031209, U2038105, and U1831207), the National Key Research and Development Program of China (Grant Nos. 2019YFA0405100, 2017YFA0402602, 2018YFA0404204, and 2016YFA0400801), Key Research Program of the Chinese Academy of Sciences (Grant No. QYZDJ-SSW-SLH021), Natural Science Foundation of Jiangsu Province (Grant No. BK20211000), Cultivation Project for FAST Scientific Payoff and Research Achievement of CAMS-CAS, the Strategic Priority Research Program on Space Science, the Western Light Youth Project of Chinese Academy of Sciences (Grant Nos. XDA15360000, XDA15052700, and XDB23040400), funding from the MaxPlanck Partner Group, the science research grants from the China Manned Space Project (Grant Nos. CMS-CSST-2021-B11 and CMS-CSST-2021-A11), and PKU development (Grant No. 7101502590). KJL acknowledges support from the XPLORER PRIZE. BBZ is supported by Fundamental Research Funds for the Central Universities (Grant No. 14380046) and the Program for Innovative Talents, Entrepreneur in Jiangsu.

Atlas of dynamic spectra of fast radio burst FRB 20201124A

Bo-Jun Wang(王铂钧)1,2,3, Heng Xu(胥恒)2, Jin-Chen Jiang(姜金辰)2, Jiang-Wei Xu(徐江伟)1,2,3, Jia-Rui Niu(牛佳瑞)2,4, Ping Chen(陈平)1,3,5, Ke-Jia Lee(李柯伽)1,2,†, Bing Zhang(张冰)6,7,‡, Wei-Wei Zhu(朱炜玮)2,§, Su-Bo Dong(东苏勃)1, Chun-Feng Zhang(张春风)2, Hai Fu(傅海)8, De-Jiang Zhou(周德江)2,4, Yong-Kun Zhang(张永坤)2,4, Pei Wang(王培)2, Yi Feng(冯毅)2,9, Ye Li(李晔)10, Dong-Zi Li(李冬子)11, Wen-Bin Lu(鲁文宾)12, Yuan-Pei Yang(杨元培)13, R. N. Caballero1,3, Ce Cai(蔡策)14, Mao-Zheng Chen(陈卯蒸)15, Zi-Gao Dai(戴子高)16, A. Esamdin(艾力·伊沙木丁)15, Heng-Qian Gan(甘恒谦)2, Jin-Lin Han(韩金林)2, Long-Fei Hao(郝龙飞)17, Yu-Xiang Huang(黄玉祥)17, Peng Jiang(姜鹏)2, Cheng-Kui Li(李承奎)14, Di Li(李菂)2,18, Hui Li(李辉)2, Xin-Qiao Li(李新乔)14, Zhi-Xuan Li(李志玄)17, Zhi-Yong Liu(刘志勇)15, Rui Luo(罗睿)19, Yun-Peng Men(门云鹏)20, Chen-Hui Niu(牛晨辉)2, Wen-Xi Peng(彭文溪)14, Lei Qian(钱磊)2, Li-Ming Song(宋黎明)14, Jing-Hai Sun(孙京海)2, Fa-Yin Wang(王发印)21, Min Wang(汪敏)17, Na Wang(王娜)15, Wei-Yang Wang(王维扬)3, Xue-Feng Wu(吴雪峰)10, Shuo Xiao(肖硕)14, Shao-Lin Xiong(熊少林)14, Yong-Hua Xu(徐永华)17, Ren-Xin Xu(徐仁新)1,3,22, Jun Yang(杨俊)21, Xuan Yang(杨轩)10, Rui Yao(姚蕊)2, Qi-Bin Yi(易祁彬)14, You-Ling Yue(岳友岭)2, Dong-Jun Yu(于东俊)2, Wen-Fei Yu(余文飞)23, Jian-Ping Yuan(袁建平)15, Bin-Bin Zhang(张彬彬)21,24, Song-Bo Zhang(张松波)10, Shuang-Nan Zhang(张双南)14, Yi Zhao(赵一)14, Wei-Kang Zheng(郑伟康)12, Yan Zhu(朱岩)2, and Jin-Hang Zou(邹金航)21,25   

  1. 1 Kavli Institute for Astronomy and Astrophysics, Peking University, Beijing 100871, China;
    2 National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100101, China;
    3 Department of Astronomy, Peking University, Beijing 100871, China;
    4 University of Chinese Academy of Sciences, Chinese Academy of Sciences, Beijing 100049, China;
    5 Department of Particle Physics and Astrophysics, Weizmann Institute of Science, Rehovot 76100, Israel;
    6 Nevada Center for Astrophysics, University of Nevada, Las Vegas, NV 89154, USA;
    7 Department of Physics and Astronomy, University of Nevada, Las Vegas, NV 89154, USA;
    8 Department of Physics & Astronomy, University of Iowa, Iowa City, IA 52242, USA;
    9 Zhejiang Laboratory, Hangzhou, Zhejiang 311121, China;
    10 Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210008, China;
    11 TAPIR, Walter Burke Institute for Theoretical Physics, Mail Code 350-17, Caltech, Pasadena, CA 91125, USA;
    12 Department of Astronomy, University of California at Berkeley, Berkeley, CA 94720, USA;
    13 South-Western Institute For Astronomy Research, Yunnan University, Yunnan 650504, China;
    14 Key Laboratory of Particle Astrophysics, Institute of High Energy Physics, Chinese Academy of Sciences, Beijing 100049, China;
    15 Xinjiang Astronomical Observatory, Chinese Academy of Sciences, Urumqi 830011, China;
    16 University of Science and Technology of China, Anhui 230026, China;
    17 Yunnan Observatories, Chinese Academy of Sciences, Kunming 650216, China;
    18 Guizhou Normal University, Guiyang 550001, China;
    19 CSIRO Space and Astronomy, Epping, NSW 1710, Australia;
    20 Max-Planck institut für Radioastronomie, Auf Dem Hügel, Bonn, 53121, Germany;
    21 School of Astronomy and Space Science, Nanjing University, Nanjing 210093, China;
    22 State Key Laboratory of Nuclear Physics and Technology, School of Physics, Peking University, Beijing 100871, China;
    23 Shanghai Astronomical Observatory, Chinese Academy of Sciences, Shanghai 200030, China;
    24 Key Laboratory of Modern Astronomy and Astrophysics (Nanjing University), Ministry of Education, Nanjing 210093, China;
    25 College of Physics, Hebei Normal University, Shijiazhuang 050024, China
  • Received:2022-10-04 Revised:2022-11-16 Accepted:2022-12-02 Online:2023-01-10 Published:2023-01-31
  • Contact: Ke-Jia Lee, Bing Zhang, Wei-Wei Zhu E-mail:kjlee@pku.edu.cn;bing.zhang@unlv.edu;zhuww@nao.cas.cn
  • Supported by:
    This work made use of data from the FAST. FAST is a Chinese national megascience facility, built and operated by the National Astronomical Observatories, Chinese Academy of Sciences. We acknowledge the use of public data from the Fermi Science Support Center (FSSC). This work is supported by the National SKA Program of China (Grant Nos. 2020SKA0120100 and 2020SKA0120200), the National Natural Science Foundation of China (Grant Nos. 12041304, 11873067, 11988101, 12041303, 11725313, 11725314, 11833003, 12003028, 12041306, 12103089, U2031209, U2038105, and U1831207), the National Key Research and Development Program of China (Grant Nos. 2019YFA0405100, 2017YFA0402602, 2018YFA0404204, and 2016YFA0400801), Key Research Program of the Chinese Academy of Sciences (Grant No. QYZDJ-SSW-SLH021), Natural Science Foundation of Jiangsu Province (Grant No. BK20211000), Cultivation Project for FAST Scientific Payoff and Research Achievement of CAMS-CAS, the Strategic Priority Research Program on Space Science, the Western Light Youth Project of Chinese Academy of Sciences (Grant Nos. XDA15360000, XDA15052700, and XDB23040400), funding from the MaxPlanck Partner Group, the science research grants from the China Manned Space Project (Grant Nos. CMS-CSST-2021-B11 and CMS-CSST-2021-A11), and PKU development (Grant No. 7101502590). KJL acknowledges support from the XPLORER PRIZE. BBZ is supported by Fundamental Research Funds for the Central Universities (Grant No. 14380046) and the Program for Innovative Talents, Entrepreneur in Jiangsu.

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摘要： Fast radio bursts (FRBs) are highly dispersed millisecond-duration radio bursts,[1,2] of which the physical origin is still not fully understood. FRB 20201124A is one of the most actively repeating FRBs. In this paper, we present the collection of 1863 burst dynamic spectra of FRB 20201124A measured with the Five-hundred-meter Aperture Spherical radio Telescope (FAST). The current collection, taken from the observation during the FRB active phase from April to June 2021, is the largest burst sample detected for any FRB so far. The standard PSRFITs format is adopted, including dynamic spectra of the burst, and the time information of the dynamic spectra, in addition, mask files help readers to identify the pulse positions are also provided. The dataset is available in Science Data Bank, with the link https://www.doi.org/10.57760/sciencedb.j00113.00076.

关键词: fast radio burst, FAST

Abstract: Fast radio bursts (FRBs) are highly dispersed millisecond-duration radio bursts,[1,2] of which the physical origin is still not fully understood. FRB 20201124A is one of the most actively repeating FRBs. In this paper, we present the collection of 1863 burst dynamic spectra of FRB 20201124A measured with the Five-hundred-meter Aperture Spherical radio Telescope (FAST). The current collection, taken from the observation during the FRB active phase from April to June 2021, is the largest burst sample detected for any FRB so far. The standard PSRFITs format is adopted, including dynamic spectra of the burst, and the time information of the dynamic spectra, in addition, mask files help readers to identify the pulse positions are also provided. The dataset is available in Science Data Bank, with the link https://www.doi.org/10.57760/sciencedb.j00113.00076.

Key words: fast radio burst, FAST

中图分类号:  (Radio sources)

  • 98.70.Dk
98.62.Nx (Jets and bursts; galactic winds and fountains) 97.60.Jd (Neutron stars)