Abstract
Abstract We report the discovery of a highly dispersed fast radio burst (FRB), FRB 181123, from an analysis of ∼1500 hr of drift scan survey data taken using the Five-hundred-meter Aperture Spherical radio Telescope (FAST). The pulse has three distinct emission components, which vary with frequency across our 1.0–1.5 GHz observing band. We measure the peak flux density to be >0.065 Jy and the corresponding fluence >0.2 Jy ms. Based on the observed dispersion measure of 1812 cm−3 pc, we infer a redshift of ∼1.9. From this, we estimate the peak luminosity and isotropic energy to be ≲2 × 1043 erg s−1 and ≲2 × 1040 erg, respectively. With only one FRB from the survey detected so far, our constraints on the event rate are limited. We derive a 95% confidence lower limit for the event rate of 900 FRBs per day for FRBs with fluences >0.025 Jy ms. We performed follow-up observations of the source with FAST for four hours and have not found a repeated burst. We discuss the implications of this discovery for our understanding of the physical mechanisms of FRBs.
Highlights
Fast Radio Bursts (FRBs) are bright millisecondduration radio bursts that are cosmological in origin
FRB came from the direction of l = 184 .06, b = −13 .47 with a positional uncertainty of 3’ based on the full width of the Five-hundred-meter Aperture Spherical radio Telescope (FAST) beam at the center frequency of 1250 MHz
The observed dispersion measure (DMs) for this FRB (1812 pc cm−3) is substantially greater than the maximum DM expected from the Galaxy in this direction ∼ 150 pc cm−3
Summary
Weiwei Zhu1,6*, Di Li1*, Rui Luo, Chenchen Miao, Bing Zhang, Laura Spitler, Duncan Lorimer, Michael Kramer, David Champion, Youling Yue, Andrew Cameron, Marilyn Cruces, Ran Duan, Yi Feng, Jun Han, George Hobbs, Chenhui Niu, Jiarui Niu, Zhichen Pan, Lei Qian, Dai Shi, Ningyu Tang, Pei Wang, Hongfeng Wang, Mao Yuan, Lei Zhang, Xinxin Zhang, Shuyun Cao, Li Feng, Hengqian Gan, Long Gao, Xuedong Gu1, Minglei Guo, Qiaoli Hao, Lin Huang, Menglin Huang, Peng Jiang, Chengjin Jin, Hui Li1, Qi Li1, Qisheng Li1, Hongfei Liu, Gaofeng Pan, Bo Peng, Hui Qian, Xiangwei Shi, Jinyuo Song, Liqiang Song, Caihong Sun, Jinghai Sun, Hong Wang, Qiming Wang, Yi Wang, Xiaoyao Xie, Jun Yan, Li Yang, Shimo Yang, Rui Yao, Dongjun Yu1, Jinglong Yu1, Chengmin Zhang, Haiyan Zhang, Shuxin Zhang, Xiaonian Zheng, Aiying Zhou, Boqin Zhu, Lichun Zhu, Ming Zhu, Wenbai Zhu, Yan Zhu CAS Key Laboratory of FAST, NAOC, Chinese Academy of Sciences, Beijing 100101, China; 2 University of Chinese Academy of Sciences, Beijing 100049, China 3 CSIRO Astronomy and Space Science, PO Box 76, Epping, NSW 1710, Australia 4 Department of Physics and Astronomy, University of Nevada, Las Vegas, Las Vegas, NV 89154, USA 5 National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100012, China 6 Max-Planck-Institut fr Radioastronomie, Auf dem Hgel 69, D-53121 Bonn, Germany 7 Department of Physics and Astronomy, West Virginia University, P.O. Box 6315, Morgantown, WV 26506, USA 8 Center for Gravitational Waves and Cosmology, Chestnut Ridge Research Building, Morgantown, WV 26505, USA 9 Image Processing and Pattern Recognition Laboratory, School of Artificial Intelligence, Beijing Normal University, Beijing 100875, China; School of Information Management, Dezhou University, Dezhou 253023, China; Institute for Astronomical Science, Dezhou University, Dezhou 253023, China; National Astronomical Data Center, Beijing 100101, China; Draft version April 30, 2020
Sign-in/Register to view highlights & summary Sign-in/Register to access full text options 
Talk to us
Join us for a 30 min session where you can share your feedback and ask us any queries you have
Schedule a callDisclaimer: All third-party content on this website/platform is and will remain the property of their respective owners and is provided on "as is" basis without any warranties, express or implied. Use of third-party content does not indicate any affiliation, sponsorship with or endorsement by them. Any references to third-party content is to identify the corresponding services and shall be considered fair use under The CopyrightLaw.
