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A repeating fast radio burst associated with a persistent radio source.
Niu, C-H; Aggarwal, K; Li, D; Zhang, X; Chatterjee, S; Tsai, C-W; Yu, W; Law, C J; Burke-Spolaor, S; Cordes, J M; Zhang, Y-K; Ocker, S K; Yao, J-M; Wang, P; Feng, Y; Niino, Y; Bochenek, C; Cruces, M; Connor, L; Jiang, J-A; Dai, S; Luo, R; Li, G-D; Miao, C-C; Niu, J-R; Anna-Thomas, R; Sydnor, J; Stern, D; Wang, W-Y; Yuan, M; Yue, Y-L; Zhou, D-J; Yan, Z; Zhu, W-W; Zhang, B.
Afiliação
  • Niu CH; National Astronomical Observatories, Chinese Academy of Sciences, Beijing, China.
  • Aggarwal K; Department of Physics and Astronomy, West Virginia University, Morgantown, WV, USA.
  • Li D; Center for Gravitational Waves and Cosmology, West Virginia University, Morgantown, WV, USA.
  • Zhang X; National Astronomical Observatories, Chinese Academy of Sciences, Beijing, China. dili@nao.cas.cn.
  • Chatterjee S; University of Chinese Academy of Sciences, Beijing, China. dili@nao.cas.cn.
  • Tsai CW; Research Center for Intelligent Computing Platforms, Zhejiang Laboratory, Hangzhou, China. dili@nao.cas.cn.
  • Yu W; University of Chinese Academy of Sciences, Beijing, China.
  • Law CJ; Shanghai Astronomical Observatory, Chinese Academy of Sciences, Shanghai, China.
  • Burke-Spolaor S; Cornell Center for Astrophysics and Planetary Science, and Department of Astronomy, Cornell University, Ithaca, NY, USA.
  • Cordes JM; National Astronomical Observatories, Chinese Academy of Sciences, Beijing, China.
  • Zhang YK; Shanghai Astronomical Observatory, Chinese Academy of Sciences, Shanghai, China. wenfei@shao.ac.cn.
  • Ocker SK; Cahill Center for Astronomy and Astrophysics, California Institute of Technology, Pasadena, CA, USA. claw@astro.caltech.edu.
  • Yao JM; Owens Valley Radio Observatory, California Institute of Technology, Big Pine, CA, USA. claw@astro.caltech.edu.
  • Wang P; Department of Physics and Astronomy, West Virginia University, Morgantown, WV, USA.
  • Feng Y; Center for Gravitational Waves and Cosmology, West Virginia University, Morgantown, WV, USA.
  • Niino Y; Canadian Institute for Advanced Research, Toronto, Ontario, Canada.
  • Bochenek C; Cornell Center for Astrophysics and Planetary Science, and Department of Astronomy, Cornell University, Ithaca, NY, USA.
  • Cruces M; National Astronomical Observatories, Chinese Academy of Sciences, Beijing, China.
  • Connor L; University of Chinese Academy of Sciences, Beijing, China.
  • Jiang JA; Cornell Center for Astrophysics and Planetary Science, and Department of Astronomy, Cornell University, Ithaca, NY, USA.
  • Dai S; Xinjiang Astronomical Observatory, Chinese Academy of Sciences, Urumqi, China.
  • Luo R; National Astronomical Observatories, Chinese Academy of Sciences, Beijing, China.
  • Li GD; National Astronomical Observatories, Chinese Academy of Sciences, Beijing, China.
  • Miao CC; University of Chinese Academy of Sciences, Beijing, China.
  • Niu JR; Research Center for Intelligent Computing Platforms, Zhejiang Laboratory, Hangzhou, China.
  • Anna-Thomas R; Institute of Astronomy, Graduate School of Science, The University of Tokyo, Tokyo, Japan.
  • Sydnor J; Research Center for the Early Universe, The University of Tokyo, Tokyo, Japan.
  • Stern D; Cahill Center for Astronomy and Astrophysics, California Institute of Technology, Pasadena, CA, USA.
  • Wang WY; Max-Planck-Institut für Radioastronomie, Bonn, Germany.
  • Yuan M; Cahill Center for Astronomy and Astrophysics, California Institute of Technology, Pasadena, CA, USA.
  • Yue YL; Kavli Institute for the Physics and Mathematics of the Universe (WPI), The University of Tokyo, Kashiwa, Japan.
  • Zhou DJ; CSIRO Space and Astronomy, Epping, New South Wales, Australia.
  • Yan Z; School of Science, Western Sydney University, Penrith South DC, New South Wales, Australia.
  • Zhu WW; CSIRO Space and Astronomy, Epping, New South Wales, Australia.
  • Zhang B; National Astronomical Observatories, Chinese Academy of Sciences, Beijing, China.
Nature ; 606(7916): 873-877, 2022 06.
Article em En | MEDLINE | ID: mdl-35676486
ABSTRACT
The dispersive sweep of fast radio bursts (FRBs) has been used to probe the ionized baryon content of the intergalactic medium1, which is assumed to dominate the total extragalactic dispersion. Although the host-galaxy contributions to the dispersion measure appear to be small for most FRBs2, in at least one case there is evidence for an extreme magneto-ionic local environment3,4 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 [Formula see text] parsecs per cubic centimetre, which is nearly an order of magnitude higher than the average of FRB host galaxies2,6, far exceeds the dispersion-measure contribution of the intergalactic medium. Caution is thus warranted in inferring redshifts for FRBs without accurate host-galaxy identifications.
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Texto completo: 1 Coleções: 01-internacional Base de dados: MEDLINE Tipo de estudo: Risk_factors_studies Idioma: En Revista: Nature Ano de publicação: 2022 Tipo de documento: Article País de afiliação: China
Texto completo
Imprimir
XML
PubMed Links
Buscar no Google

Texto completo: 1 Coleções: 01-internacional Base de dados: MEDLINE Tipo de estudo: Risk_factors_studies Idioma: En Revista: Nature Ano de publicação: 2022 Tipo de documento: Article País de afiliação: China