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A repeating fast radio burst associated with a persistent radio source

Niu, C.-H. and Aggarwal, K. and Li, D. and Zhang, X. and Chatterjee, S. and Tsai, C.-W. and Yu, W. and Law, C. J. and Burke-Spolaor, S. and Cordes, J. M. and Zhang, Y.-K. and Ocker, S. K. and Yao, J.-M. and Wang, P. and Feng, Y. and Niino, Y. and Bochenek, C. and Cruces, M. and Connor, L. and Jiang, J.-A. and Dai, S. and Luo, R. and Li, G.-D. and Miao, C.-C. and Niu, J.-R. and Anna-Thomas, R. and Sydnor, J. and Stern, D. and Wang, W.-Y. and Yuan, M. and Yue, Y.-L. and Zhou, D.-J. and Yan, Z. and Zhu, W.-W. and Zhang, B. (2022) A repeating fast radio burst associated with a persistent radio source. Nature, 606 (7916). pp. 873-877. ISSN 0028-0836. doi:10.1038/s41586-022-04755-5. https://resolver.caltech.edu/CaltechAUTHORS:20220617-151636567

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[img] Image (JPEG) (Extended Data Fig. 2: Spectrum of the PRS associated with FRB 20190520B) - Supplemental Material
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[img] Image (JPEG) (Extended Data Fig. 3: Optical spectrum of the FRB 20190520B host galaxy obtained at Palomar) - Supplemental Material
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[img] Image (JPEG) (Extended Data Fig. 4: Posterior probability distributions) - Supplemental Material
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[img] Image (JPEG) (Extended Data Fig. 5: The fluence-width distribution at 1.25 GHz for FRB 20190520B) - Supplemental Material
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[img] Image (JPEG) (Extended Data Fig. 6: The distribution of burst energies for FRB 20190520B) - Supplemental Material
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Abstract

The dispersive sweep of fast radio bursts (FRBs) has been used to probe the ionized baryon content of the intergalactic medium, which is assumed to dominate the total extragalactic dispersion. Although the host-galaxy contributions to the dispersion measure appear to be small for most FRBs, in at least one case there is evidence for an extreme magneto-ionic local environment and a compact persistent radio source5. Here we report the detection and localization of the repeating FRB 20190520B, which is co-located with a compact, persistent radio source and associated with a dwarf host galaxy of high specific-star-formation rate at a redshift of 0.241 ± 0.001. The estimated host-galaxy dispersion measure of approximately 903⁺⁷²₋₁₁₁ parsecs per cubic centimetre, which is nearly an order of magnitude higher than the average of FRB host galaxies, far exceeds the dispersion-measure contribution of the intergalactic medium. Caution is thus warranted in inferring redshifts for FRBs without accurate host-galaxy identifications.


Item Type:Article
Related URLs:
URLURL TypeDescription
https://doi.org/10.1038/s41586-022-04755-5DOIArticle
https://arxiv.org/abs/2110.07418arXivDiscussion Paper
https://doi.org/10.11922/sciencedb.o00069.00004DOIFAST data
https://doi.org/10.7910/DVN/C5CEEIDOIVLA data
https://github.com/peterniuzai/FRB190520B_discovery_paper_Code_availability.gitRelated ItemData analysis code
https://github.com/realfastvla/rfpipeRelated ItemCode relevant to the analysis of the VLA observations
ORCID:
AuthorORCID
Tsai, C.-W.0000-0002-9390-9672
Law, C. J.0000-0002-4119-9963
Bochenek, C.0000-0003-3875-9568
Connor, L.0000-0002-7587-6352
Stern, D.0000-0003-2686-9241
Alternate Title:A repeating FRB in a dense environment with a compact persistent radio source
Additional Information:© The Author(s) 2022. This article is licensed under a Creative Commons Attribution 4.0 International License, which permits use, sharing, adaptation, distribution and reproduction in any medium or format, as long as you give appropriate credit to the original author(s) and the source, provide a link to the Creative Commons license, and indicate if changes were made. The images or other third party material in this article are included in the article’s Creative Commons license, unless indicated otherwise in a credit line to the material. If material is not included in the article’s Creative Commons license and your intended use is not permitted by statutory regulation or exceeds the permitted use, you will need to obtain permission directly from the copyright holder. To view a copy of this license, visit http://creativecommons.org/licenses/by/4.0/. Received 23 July 2021; Accepted 11 April 2022; Published 08 June 2022. This work was supported by National Natural Science Foundation of China (NSFC)programme numbers 11988101, 11725313, 12041303, U1731238, U2031117, U1831131 and U1831207, and by the Cultivation Project for FAST Scientific Payoff and Research Achievement of CAMS-CAS. C.-H.N. acknowledges support from the FAST Fellowship. S.C., J.M.C. and S.O. acknowledge support from the National Science Foundation (AAG 1815242) and are members of the NANOGrav Physics Frontiers Center, which is supported by NSF award PHY-1430284. C.J.L. acknowledges support from the National Science Foundation under grant number 2022546. K.A., S.B.-S. and R.A.-T. acknowledge support from NSF grant AAG-1714897. P.W. thanks the YSBR-006, CAS Project for Young Scientists in Basic Research. S.B.-S. is a CIFAR Azrieli Global Scholar in the Gravity and the Extreme Universe programme. Y.N. acknowledges support from JSPS KAKENHI grant number JP20H01942. J.-A.J. acknowledges support from the Japan Society for the Promotion of Science (JSPS) KAKENHI grant JP19K23456 and JP18J12714. S.D. is the recipient of an Australian Research Council Discovery Early Career Award (DE210101738) funded by the Australian Government. We thank the FAST key science project for supporting follow-up observations; and the FAST collaborations and realfast team for their technical support. Some data presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California and the National Aeronautics and Space Administration. The observatory was made possible by the generous financial support of the W. M. Keck Foundation. This study is based in part on data collected at the Subaru Telescope, which is operated by the National Astronomical Observatory of Japan. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. This work was supported by the China Science and Technology Cloud (CSTCloud) and China Environment for Network Innovations (CENI). We thank the staff of CSTCloud/CENI for their support during data processing. Data availability: The FAST data are available at https://doi.org/10.11922/sciencedb.o00069.00004. The VLA data can be accessed at https://doi.org/10.7910/DVN/C5CEEI. Code availability: The data analysis code used for FAST observations is available at https://github.com/peterniuzai/FRB190520B_discovery_paper_Code_availability.git. For code relevant to the analysis of the VLA observations, see https://github.com/realfastvla/rfpipe. The publicly available packages CASA, Heimdall and DM_phase can be found on their respective websites. These authors contributed equally: C.-H. Niu, K. Aggarwal, D. Li. Contributions: C.H.N. discovered the source FRB 20190520B. D.L., C.J.L., S.C., C.-W.T., W.Y. and C.-H.N. initiated the follow-up projects. D.L., C.-H.N., B.Z. and W.-W.Z. led the follow-up FAST observations. C.-H.N., J.-M.Y., Y.-K.Z., P.W., D.-J.Z. and Y.F. searched and processed the FAST data. K.A., C.J.L., S.C., X.Z., S.B.-S., Z.Y., W.Y. and L.C. contributed to the VLA burst detection and localization, identification and measurements of the associated persistent radio source. C.-W.T., S.C., D.S., Y.N., J.-A.J., C.B. and G.-D.L. contributed to the optical/NIR follow-up observations and analysis. S.K.O., J.M.C., S.C., J.-M.Y. and C.-H.N. measured the burst scattering and analysed the propagation effects. J.M.C., B.Z. and W.-Y.W. contributed to the DMhost estimation. K.A., Y.-K.Z., J.-R.N., R.L., W.-W.Z. and C.-H.N. contributed to the periodicity and burst rate analysis. P.W. and Y.-K.Z. helped with energy calibration and M.Y. contributed to the radio frequency interference removal on FAST data. Z.Y., W.Y., M.C., S.D. and Y.-L.Y. contributed to other follow-up observations. S.B.-S., D.L., K.A., C.-H.N., S.C., J.M.C., S.K.O. and C.J.L. had major contributions to the preparation of the manuscript. All of the authors have reviewed, discussed and commented on the presented results and the manuscript. The authors declare no competing interests. Peer review information: Nature thanks Adam Deller and Jason Hessels for their contribution to the peer review of this work. Peer reviewer reports are available.
Group:Infrared Processing and Analysis Center (IPAC)
Funders:
Funding AgencyGrant Number
National Natural Science Foundation of China11988101
National Natural Science Foundation of China11725313
National Natural Science Foundation of China12041303
National Natural Science Foundation of ChinaU1731238
National Natural Science Foundation of ChinaU2031117
National Natural Science Foundation of ChinaU1831131
National Natural Science Foundation of ChinaU1831207
FAST FellowshipUNSPECIFIED
NSFAAG-1815242
NSFPHY-1430284
NSFAST-2022546
NSFAAG-1714897
Chinese Academy of SciencesYSBR-006
Canadian Institute for Advanced Research (CIFAR)UNSPECIFIED
Japan Society for the Promotion of Science (JSPS)JP20H01942
Japan Society for the Promotion of Science (JSPS)JP19K23456
Japan Society for the Promotion of Science (JSPS)JP18J12714
Australian Research CouncilDE210101738
W. M. Keck FoundationUNSPECIFIED
China Science and Technology CloudUNSPECIFIED
China Environment for Network InnovationsUNSPECIFIED
Issue or Number:7916
DOI:10.1038/s41586-022-04755-5
Record Number:CaltechAUTHORS:20220617-151636567
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20220617-151636567
Official Citation:Niu, CH., Aggarwal, K., Li, D. et al. A repeating fast radio burst associated with a persistent radio source. Nature 606, 873–877 (2022). https://doi.org/10.1038/s41586-022-04755-5
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:115195
Collection:CaltechAUTHORS
Deposited By: Tony Diaz
Deposited On:17 Jun 2022 19:29
Last Modified:12 Jul 2022 21:43

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