Xu, H. and Niu, J. R. and Chen, P. and Lee, K. J. and Zhu, W. W. and Dong, S. and Zhang, B. and Jiang, J. C. and Wang, B. J. and Xu, J. W. and Zhang, C. F. and Fu, H. and Filippenko, A. V. and Peng, E. W. and Zhou, D. J. and Zhang, Y. K. and Wang, P. and Li, Y. and Feng, Y. and Brink, T. G. and Li, D. Z. and Lu, W. and Yang, Y. P. and Caballero, R. N. and Cai, C. and Chen, M. Z. and Dai, Z. G. and Djorgovski, S. G. and Esamdin, A. and Gan, H. Q. and Guhathakurta, P. and Han, J. L. and Hao, L. F. and Huang, Y. X. and Jiang, P. and Li, C. K. and Li, D. and Li, H. and Li, X. Q. and Li, Z. X. and Liu, Z. Y. and Luo, R. and Men, Y. P. and Niu, C. H. and Peng, W. X. and Qian, L. and Song, L. M. and Stern, D. and Stockton, A. and Sun, J. H. and Wang, F. Y. and Wang, M. and Wang, N. and Wang, W. Y. and Wu, X. F. and Xiao, S. and Xiong, S. L. and Xu, Y. H. and Xu, R. X. and Yang, J. and Yang, X. and Yao, R. and Yi, Q. B. and Yue, Y. L. and Yu, D. J. and Yu, W. F. and Yuan, J. P. and Zhang, B. B. and Zhang, S. B. and Zhang, S. N. and Zhao, Y. and Zheng, W. K. and Zhu, Y. and Zou, J. H. (2021) A fast radio burst source at a complex magnetised site in a barred galaxy. . (Unpublished) https://resolver.caltech.edu/CaltechAUTHORS:20220224-200826034
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Abstract
Fast radio bursts (FRBs) are highly dispersed radio bursts prevailing in the universe. The recent detection of FRB~200428 from a Galactic magnetar suggested that at least some FRBs originate from magnetars, but it is unclear whether the majority of cosmological FRBs, especially the actively repeating ones, are produced from the magnetar channel. Here we report the detection of 1863 polarised bursts from the repeating source FRB~20201124A during a dedicated radio observational campaign of Five-hundred-meter Aperture Spherical radio Telescope (FAST). The large sample of radio bursts detected in 88 hr over 54 days indicate a significant, irregular, short-time variation of the Faraday rotation measure (RM) of the source during the first 36 days, followed by a constant RM during the later 18 days. Significant circular polarisation up to 75% was observed in a good fraction of bursts. Evidence suggests that some low-level circular polarisation originates from the conversion from linear polarisation during the propagation of the radio waves, but an intrinsic radiation mechanism is required to produce the higher degree of circular polarisation. All of these features provide evidence for a more complicated, dynamically evolving, magnetised immediate environment around this FRB source. Its host galaxy was previously known. Our optical observations reveal that it is a Milky-Way-sized, metal-rich, barred-spiral galaxy at redshift z = 0.09795 ± 0.00003, with the FRB source residing in a low stellar density, interarm region at an intermediate galactocentric distance, an environment not directly expected for a young magnetar formed during an extreme explosion of a massive star.
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| Additional Information: | Attribution 4.0 International (CC BY 4.0). This work made use of data from the FAST. FAST is a Chinese national mega-science 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 National SKA Program of China (2020SKA0120100, 2020SKA0120200), Natural Science Foundation of China (12041304, 11873067, 11988101, 12041303, 11725313, 11725314, 11833003, 12003028, 12041306, 12103089, U2031209, U2038105, U1831207), National Program on Key Research and Development Project (2019YFA0405100, 2017YFA0402602 ,2018YFA0404204, 2016YFA0400801), Key Research Program of the CAS (QYZDJ-SSW-SLH021), Natural Science Foundation of Jiangsu Province (BK20211000), Cultivation Project for FAST Scientific Payoff and Research Achievement of CAMS-CAS, the Strategic Priority Research Program on Space Science, the Chinese Academy of Sciences (Grant No. XDA15360000, XDA15052700, XDB23040400), funding from the Max-Planck Partner Group, the science research grants from the China Manned Space Project (CMS-CSST-2021-B11,NO. CMS-CSST-2021-A11), and PKU development grant 7101502590. AVF’s group at U.C. Berkeley is supported by the Christopher R. Redlich Fund, the Miller Institute for Basic Research in Science (in which A.V.F. is a Miller Senior Fellow), and many individual donors. SD acknowledges the support from the XPLORER PRIZE. BBZ acknowledges support by Fundamental Research Funds for the Central Universities (14380046), and the Program for Innovative Talents, Entrepreneur in Jiangsu. We thank the staff of W.M. Keck Observatory for their help during the observing runs. We thank L. Ho, H. Gao and R. Li for discussions. Author Contributions HX, JRN, PC led the data analysis. KJL, WWZ, SD, and BZ coordinated the observational campaign, co-supervised data analyses and interpretations, and led the paper writing. JCJ conducted the polarisation and RM measurements. BJW, JWX, CFZ, KJL did the timing analysis, periodicity search, DM measurement, burst searching, and Faraday conversion measurement. YPM contribute to the searching software developing, and RNC, MZC, LFH, YXH,ZYL, ZXL, YHX, JPY performed software testing. DJZ, YKZ,YF, CHN, FYW,XFW contributed to, radio data analysis. PC, SD, HF, AVF, EWP, TGB, SGD, PG, DS, AS, WKZ, and AE contributed to the optical observations and data reduction; AVF also edited the manuscript in detail. PC, SD, HF and YL contributed to analyzing and interpreting the optical data. PJ, HQG, JLH, JLH, HL,QL, JHS, RY, YLY, DJY, YZ aided with FAST observations. JLH, DL, MW, NW helped with observation coordination. KJL, BZ, DZL, WYW, RXX, WL,YPY,ZGD,RL provided theoretical discussions. CC, CKL, XQL, WXP, LMS, SX, SLX, JY, XY, QBY, BBZ, SNZ, JHZ contributed to the high energy observation. Data availability: Raw data are available from the FAST data center: http://fast.bao.ac.cn. Owing to the large data volume, we encourage contacting the corresponding author for the data transfer. The directly related data that support the findings of this study can be found from PSRPKU website: https://psr.pku.edu.cn/index.php/publications/frb20201124a/. Code availability: PSRCHIVE (http://psrchive.sourceforge.net); TRANSIENTX (https://github.com/ypmen/TransientX); BEAR (https://psr.pku.edu.cn/index.php/publications/frb180301/). The authors declare no competing financial interests | ||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||
| Group: | TAPIR, Walter Burke Institute for Theoretical Physics, Astronomy Department | ||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||
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| DOI: | 10.48550/arXiv.2111.11764 | ||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||
| Record Number: | CaltechAUTHORS:20220224-200826034 | ||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||
| Persistent URL: | https://resolver.caltech.edu/CaltechAUTHORS:20220224-200826034 | ||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||
| Usage Policy: | No commercial reproduction, distribution, display or performance rights in this work are provided. | ||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||
| ID Code: | 113584 | ||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||
| Collection: | CaltechAUTHORS | ||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||
| Deposited By: | George Porter | ||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||
| Deposited On: | 28 Feb 2022 16:16 | ||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||
| Last Modified: | 02 Jun 2023 01:20 |
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