NAOC Open IR
Constraining the transient high-energy activity of FRB 180916.J0158+65 with Insight-HXMT follow-up observations
Guidorzi, C.1,2,3; Orlandini, M.3; Frontera, F.1,3; Nicastro, L.3; Xiong, S. L.4; Liao, J. Y.4; Li, G.4; Zhang, S. N.4,5; Amati, L.3; Virgilli, E.3; Zhang, S.4; Bu, Q. C.4; Cai, C.4,5; Cao, X. L.4; Chang, Z.4; Chen, L.6; Chen, T. X.4; Chen, Y.4; Chen, Y. P.4; Cui, W. W.4; Du, Y. Y.4; Gao, G. H.4,5; Gao, H.4,5; Gao, M.4; Ge, M. Y.4; Gu, Y. D.4; Guan, J.4; Guo, C. C.4,5; Han, D. W.4; Huang, Y.4; Huo, J.4; Jia, S. M.4; Jiang, W. C.4; Jin, J.4; Kong, L. D.4,5; Li, B.4; Li, C. K.4; Li, T. P.4,5,7; Li, W.4; Li, X.4; Li, X. B.4; Li, X. F.4; Li, Z. W.4; Liang, X. H.4; Liu, B. S.4; Liu, C. Z.4; Liu, H. X.4,5; Liu, H. W.4; Liu, X. J.4; Lu, F. J.4; Lu, X. F.4; Luo, Q.4; Luo, T.4; Ma, R. C.4,5; Ma, X.4; Meng, B.4; Nang, Y.4,5; Nie, J. Y.4; Ou, G.8; Qu, J. L.4; Ren, X. Q.4,5; Sai, N.4,5; Song, L. M.4,5; Song, X. Y.4; Sun, L.4; Tan, Y.4; Tao, L.4; Tuo, Y. L.4,5; Wang, C.5,9; Wang, L. J.4; Wang, P. J.4,5; Wang, W. S.8; Wang, Y. S.4; Wen, X. Y.4; Wu, B. Y.4,5; Wu, B. B.4; Wu, M.4; Xiao, G. C.4,5; Xiao, S.4,5; Xu, Y. P.4,5; Yang, R.10; Yang, S.4; Yang, Y. J.4; Yi, Q. B.4,11; Yin, Q. Q.4; You, Y.4,5; Zhang, F.4; Zhang, H. M.8; Zhang, J.4; Zhang, P.4; Zhang, W. C.4; Zhang, W.4,5; Zhang, Y. F.4; Zhang, Y. H.4,5; Zhao, H. S.4; Zhao, X. F.4,5; Zheng, S. J.4; Zheng, Y. G.4,10; Zhou, D. K.4,5
2020-10-15
Source PublicationASTRONOMY & ASTROPHYSICS
ISSN0004-6361
Volume642Pages:9
AbstractContext. A link has finally been established between magnetars and fast radio burst (FRB) sources. Within this context, a major issue that remains unresolved pertains to whether sources of extragalactic FRBs exhibit X/gamma -ray outbursts and whether this is correlated with radio activity. If so, the subsequent goal is to identify these sources.Aims. We aim to constrain possible X/gamma -ray burst activity from one of the nearest extragalactic FRB sources currently known. This is to be done over a broad energy range by looking for bursts over a range of timescales and energies that are compatible with those of powerful flares from extragalactic magnetars.Methods. We followed up on the observation of the as-yet nearest extragalactic FRB source, located at a mere 149 Mpc distance, namely, the periodic repeater FRB 180916.J0158+65. This took place during the active phase between 4 and 7 February 2020, using the Insight-Hard X-ray Modulation Telescope (Insight-HXMT). By taking advantage of the combination of broad-band wavelengths, a large effective area, and several independent detectors at our disposal, we searched for bursts over a set of timescales from 1 ms to 1.024 s with a sensitive algorithm that had been previously characterised and optimised. Moreover, through simulations, we studied the sensitivity of our technique in the released energy-duration phase space for a set of synthetic flares and assuming a range of different energy spectra.Results. We constrain the possible occurrence of flares in the 1-100 keV energy band to E< 10(46) erg for durations t< 0.1 s over several tens of ks exposure.Conclusions. We can rule out the occurrence of giant flares similar to the ones that were observed in the few cases of Galactic magnetars. The absence of reported radio activity during our observations prevents us from making any determinations regarding the possibility of simultaneous high-energy emission.
Keywordradiation mechanisms: non-thermal stars: magnetars
Funding OrganizationNational Program on Key Research and Development Project ; National Program on Key Research and Development Project ; National Natural Science Foundation of China ; National Natural Science Foundation of China ; China National Space Administration (CNSA) ; China National Space Administration (CNSA) ; Chinese Academy of Sciences (CAS) ; Chinese Academy of Sciences (CAS) ; ASI-INAF ; ASI-INAF ; National Program on Key Research and Development Project ; National Program on Key Research and Development Project ; National Natural Science Foundation of China ; National Natural Science Foundation of China ; China National Space Administration (CNSA) ; China National Space Administration (CNSA) ; Chinese Academy of Sciences (CAS) ; Chinese Academy of Sciences (CAS) ; ASI-INAF ; ASI-INAF ; National Program on Key Research and Development Project ; National Program on Key Research and Development Project ; National Natural Science Foundation of China ; National Natural Science Foundation of China ; China National Space Administration (CNSA) ; China National Space Administration (CNSA) ; Chinese Academy of Sciences (CAS) ; Chinese Academy of Sciences (CAS) ; ASI-INAF ; ASI-INAF ; National Program on Key Research and Development Project ; National Program on Key Research and Development Project ; National Natural Science Foundation of China ; National Natural Science Foundation of China ; China National Space Administration (CNSA) ; China National Space Administration (CNSA) ; Chinese Academy of Sciences (CAS) ; Chinese Academy of Sciences (CAS) ; ASI-INAF ; ASI-INAF
DOI10.1051/0004-6361/202039129
WOS KeywordSOFT-GAMMA-REPEATER ; FAST RADIO-BURSTS ; SYNCHROTRON MASER EMISSION ; GIANT FLARE ; BACKGROUND MODEL ; SGR 1900+14 ; AUGUST 27 ; BEPPOSAX ; SGR-1806-20 ; TELESCOPE
Language英语
Funding ProjectNational Program on Key Research and Development Project[2016YFA0400800] ; National Natural Science Foundation of China[11733009] ; National Natural Science Foundation of China[U1838201] ; National Natural Science Foundation of China[U1838202] ; China National Space Administration (CNSA) ; Chinese Academy of Sciences (CAS) ; ASI-INAF[2017-14-H.0]
Funding OrganizationNational Program on Key Research and Development Project ; National Program on Key Research and Development Project ; National Natural Science Foundation of China ; National Natural Science Foundation of China ; China National Space Administration (CNSA) ; China National Space Administration (CNSA) ; Chinese Academy of Sciences (CAS) ; Chinese Academy of Sciences (CAS) ; ASI-INAF ; ASI-INAF ; National Program on Key Research and Development Project ; National Program on Key Research and Development Project ; National Natural Science Foundation of China ; National Natural Science Foundation of China ; China National Space Administration (CNSA) ; China National Space Administration (CNSA) ; Chinese Academy of Sciences (CAS) ; Chinese Academy of Sciences (CAS) ; ASI-INAF ; ASI-INAF ; National Program on Key Research and Development Project ; National Program on Key Research and Development Project ; National Natural Science Foundation of China ; National Natural Science Foundation of China ; China National Space Administration (CNSA) ; China National Space Administration (CNSA) ; Chinese Academy of Sciences (CAS) ; Chinese Academy of Sciences (CAS) ; ASI-INAF ; ASI-INAF ; National Program on Key Research and Development Project ; National Program on Key Research and Development Project ; National Natural Science Foundation of China ; National Natural Science Foundation of China ; China National Space Administration (CNSA) ; China National Space Administration (CNSA) ; Chinese Academy of Sciences (CAS) ; Chinese Academy of Sciences (CAS) ; ASI-INAF ; ASI-INAF
WOS Research AreaAstronomy & Astrophysics
WOS SubjectAstronomy & Astrophysics
WOS IDWOS:000581917100005
PublisherEDP SCIENCES S A
Citation statistics
Document Type期刊论文
Identifierhttp://ir.bao.ac.cn/handle/114a11/81922
Collection中国科学院国家天文台
Corresponding AuthorGuidorzi, C.
Affiliation1.Univ Ferrara, Dept Phys & Earth Sci, Via Saragat 1, I-44122 Ferrara, Italy
2.INFN Sez Ferrara, Via Saragat 1, I-44122 Ferrara, Italy
3.INAF Osservatorio Astrofis & Sci Spazio Bologna, Via Piero Gobetti 101, I-40129 Bologna, Italy
4.Chinese Acad Sci, Inst High Energy Phys, Key Lab Particle Astrophys, 19B Yuquan Rd, Beijing 100049, Peoples R China
5.Chinese Acad Sci, Univ Chinese Acad Sci, Beijing 100049, Peoples R China
6.Beijing Normal Univ, Dept Astron, Beijing 100088, Peoples R China
7.Tsinghua Univ, Dept Astron, Beijing 100084, Peoples R China
8.Chinese Acad Sci, Inst High Energy Phys, Comp Div, 19B Yuquan Rd, Beijing 100049, Peoples R China
9.Chinese Acad Sci, Natl Astron Observ, Key Lab Space Astron & Technol, Beijing 100012, Peoples R China
10.Hebei Univ, Coll Phys Sci & Technol, 180 Wusi Dong Rd, Baoding City 071002, Hebei, Peoples R China
11.Xiangtan Univ, Sch Phys & Optoelect, Xiangtan 411105, Hunan, Peoples R China
Recommended Citation
GB/T 7714
Guidorzi, C.,Orlandini, M.,Frontera, F.,et al. Constraining the transient high-energy activity of FRB 180916.J0158+65 with Insight-HXMT follow-up observations[J]. ASTRONOMY & ASTROPHYSICS,2020,642:9.
APA Guidorzi, C..,Orlandini, M..,Frontera, F..,Nicastro, L..,Xiong, S. L..,...&Zhou, D. K..(2020).Constraining the transient high-energy activity of FRB 180916.J0158+65 with Insight-HXMT follow-up observations.ASTRONOMY & ASTROPHYSICS,642,9.
MLA Guidorzi, C.,et al."Constraining the transient high-energy activity of FRB 180916.J0158+65 with Insight-HXMT follow-up observations".ASTRONOMY & ASTROPHYSICS 642(2020):9.
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