A fast radio burst source at a complex magnetized site in a barred galaxy

被引：154

作者：

Xu, H. ^{[1
,2
,3
]}

Niu, J. R. ^{[2
,4
]}

Chen, P. ^{[1
,3
,5
]}

Lee, K. J. ^{[1
,2
]}

Zhu, W. W. ^{[2
]}

Dong, S. ^{[1
]}

Zhang, B. ^{[1
,2
]}

Jiang, J. C. ^{[1
,2
,3
]}

Wang, B. J. ^{[1
,2
,3
]}

Xu, J. W. ^{[1
,2
,3
]}

Zhang, C. F. ^{[1
,2
,3
]}

Fu, H. ^{[2
]}

Filippenko, A., V ^{[1
]}

Peng, E. W. ^{[1
,3
]}

Zhou, D. J. ^{[2
,4
]}

Zhang, Y. K. ^{[2
,4
]}

Wang, P. ^{[2
]}

Feng, Y. ^{[2
,6
]}

Li, Y. ^{[7
]}

Brink, T. G. ^{[1
]}

Li, D. Z. ^{[8
]}

Lu, W. ^{[9
]}

Yang, Y. P. ^{[10
]}

Caballero, R. N. ^{[1
]}

Cai, C. ^{[11
]}

Chen, M. Z. ^{[12
]}

Dai, Z. G. ^{[13
]}

Djorgovski, S. G. ^{[14
]}

Esamdin, A. ^{[12
]}

Gan, H. Q. ^{[2
]}

Guhathakurta, P. ^{[15
]}

Han, J. L. ^{[2
]}

Hao, L. F. ^{[16
]}

Huang, Y. X. ^{[16
]}

Jiang, P. ^{[2
]}

Li, C. K. ^{[11
]}

Li, D. ^{[2
,17
]}

Li, H. ^{[2
]}

Li, X. Q. ^{[11
]}

Li, Z. X. ^{[16
]}

Liu, Z. Y. ^{[12
]}

Luo, R. ^{[18
]}

Men, Y. P. ^{[19
]}

Niu, C. H. ^{[2
]}

Peng, W. X. ^{[11
]}

Qian, L. ^{[2
]}

Song, L. M. ^{[11
]}

Stern, D. ^{[20
]}

Stockton, A. ^{[21
]}

Sun, J. H. ^{[2
]}

机构：

[1] Peking Univ, Kavli Inst Astron & Astrophys, Beijing, Peoples R China

[2] Chinese Acad Sci, Natl Astron Observ, Beijing, Peoples R China

[3] Peking Univ, Dept Astron, Beijing, Peoples R China

[4] Chinese Acad Sci, Univ Chinese Acad Sci, Beijing, Peoples R China

[5] Weizmann Inst Sci, Dept Particle Phys & Astrophys, Rehovot, Israel

[6] Univ Nevada, Nevada Ctr Astrophys, Las Vegas, NV 89154 USA

[7] Univ Nevada, Dept Phys & Astron, Las Vegas, NV 89154 USA

[8] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA

[9] Univ Calif Berkeley, Dept Astron, 601 Campbell Hall, Berkeley, CA 94720 USA

[10] Zhejiang Lab, Hangzhou, Peoples R China

[11] Chinese Acad Sci, Purple Mt Observ, Nanjing, Peoples R China

[12] CALTECH, Walter Burke Inst Theoret Phys, TAPIR, Pasadena, CA 91125 USA

[13] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA

[14] Yunnan Univ, South Western Inst Astron Res, Kunming, Yunnan, Peoples R China

[15] Chinese Acad Sci, Inst High Energy Phys, Key Lab Particle Astrophys, Beijing, Peoples R China

[16] Chinese Acad Sci, Xinjiang Astron Observ, Urumqi, Peoples R China

[17] Univ Sci & Technol China, Hefei, Peoples R China

[18] CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA

[19] Univ Calif Santa Cruz, Dept Astron & Astrophys, UCO Lick Observ, Santa Cruz, CA 95064 USA

[20] Chinese Acad Sci, Yunnan Observ, Kunming, Yunnan, Peoples R China

[21] Guizhou Normal Univ, Guiyang, Peoples R China

[22] CSIRO Space & Astron, Epping, NSW, Australia

[23] Max Planck Inst Radioastron, Bonn, Germany

[24] CALTECH, Jet Prop Lab, Pasadena, CA USA

[25] Univ Hawaii, Inst Astron, 2680 Woodlawn Dr, Honolulu, HI 96822 USA

[26] Nanjing Univ, Sch Astron & Space Sci, Nanjing, Peoples R China

来源：

NATURE | 2022年 / 609卷 / 7928期

关键词：

FARADAY CONVERSION; EMISSION; ROTATION; POLARIZATION; RADIATION; SEARCH;

D O I：

10.1038/s41586-022-05071-8

中图分类号：

O [数理科学和化学]; P [天文学、地球科学]; Q [生物科学]; N [自然科学总论];

学科分类号：

07 ; 0710 ; 09 ;

摘要：

Fast radio bursts (FRBs) are highly dispersed, millisecond-duration radio bursts(1-3). Recent observations of a Galactic FRB4-8 suggest that at least some FRBs originate from magnetars, but the origin of cosmological FRBs is still not settled. Here we report the detection of 1,863 bursts in 82 h over 54 days from the repeating source FRB 20201124A (ref. (9)). These observations show irregular short-time variation of the Faraday rotation measure (RM), which scrutinizes the density-weighted line-of-sight magnetic field strength, of individual bursts during the first 36 days, followed by a constant RM. We detected circular polarization in more than half of the burst sample, including one burst reaching a high fractional circular polarization of 75%. Oscillations in fractional linear and circular polarizations, as well as polarization angle as a function of wavelength, were detected. All of these features provide evidence for a complicated, dynamically evolving, magnetized immediate environment within about an astronomical unit (au; Earth-Sun distance) of the source. Our optical observations of its Milky-Way-sized, metal-rich host galaxy(10-12) show a barred spiral, with the FRB source residing in a low-stellar-density interarm region at an intermediate galactocentric distance. This environment is inconsistent with a young magnetar engine formed during an extreme explosion of a massive star that resulted in a long gamma-ray burst or superluminous supernova.

引用

页码：685 / +

页数：16

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