A search for prompt γ-ray counterparts to fast radio bursts in the Insight-HXMT data
Journal
Date Issued
2020
Author(s)
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Xiong, S. L.
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Liao, J. Y.
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Li, G.
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Zhang, S. N.
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Frontera, Filippo
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Zhang, S.
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Bu, Q. C.
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Cai, C.
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Cao, X. L.
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Chang, Z.
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Chen, G.
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Chen, L.
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Chen, T. X.
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Chen, Y. B.
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Chen, Y. P.
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Cui, W.
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Cui, W. W.
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Deng, J. K.
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Dong, Y. W.
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Du, Y. Y.
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Fu, M. X.
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Gao, G. H.
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Gao, H.
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Gao, M.
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Ge, M. Y.
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Gu, Y. D.
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Guan, J.
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Guo, C. C.
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Han, D. W.
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Huang, Y.
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Huo, J.
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Jia, S. M.
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Jiang, L. H.
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Jiang, W. C.
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Jin, J.
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Jin, Y. J.
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Kong, L. D.
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Li, B.
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Li, C. K.
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Li, M. S.
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Li, T. P.
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Li, W.
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Li, X.
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Li, X. B.
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Li, X. F.
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Li, Y. G.
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Li, Z. W.
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Liang, X. H.
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Liu, B. S.
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Liu, C. Z.
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Liu, G. Q.
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Liu, H. W.
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Liu, X. J.
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Liu, Y. N.
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Lu, B.
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Lu, F. J.
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Lu, X. F.
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Luo, Q.
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Luo, T.
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Ma, R. C.
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Ma, X.
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Meng, B.
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Nang, Y.
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Nie, J. Y.
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Ou, G.
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Qu, J. L.
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Sai, N.
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Shang, R. C.
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Song, L. M.
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Song, X. Y.
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Sun, L.
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Tan, Y.
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Tao, L.
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Tuo, Y. L.
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Wang, C.
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Wang, G. F.
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Wang, J.
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Wang, W. S.
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Wang, Y. S.
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Wen, X. Y.
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Wu, B. Y.
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Wu, B. B.
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Wu, M.
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Xiao, G. C.
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Xiao, S.
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Xu, Y. P.
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Yang, J. W.
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Yang, S.
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Yang, Y. J.
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Yi, Q. B.
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Yin, Q. Q.
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You, Y.
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Zhang, A. M.
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Zhang, C. M.
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Zhang, F.
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Zhang, H. M.
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Zhang, J.
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Zhang, T.
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Zhang, W. C.
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Zhang, W.
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Zhang, W. Z.
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Zhang, Y.
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Zhang, Y. F.
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Zhang, Y. J.
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Zhang, Z.
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Zhang, Z. L.
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Zhang, H. S.
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Zhang, X. F.
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Zheng, S. J.
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Zhou, D. K.
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Zhou, J. F.
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Zhu, Y. X.
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Zhu, Y.
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Zhuang, R. L.
Abstract
Context. No robust detection of prompt electromagnetic counterparts to fast radio bursts (FRBs) has yet been obtained, in spite of several multi-wavelength searches having been carried out so far. Specifically, X/γ-rays counterparts are predicted by some models.
Aims: We aim to search for prompt γ-ray counterparts in the Insight-Hard X-ray Modulation Telescope (Insight-HXMT) data, taking advantage of the unique combination of the large effective area in the keV-MeV energy range, and of sub-ms time resolution. Methods: We selected 39 FRBs that were promptly visible from the High-Energy (HE) instrument aboard Insight-HXMT. After calculating the expected arrival times at the location of the spacecraft, we searched for a significant excess in both individual and cumulative time profiles over a wide range of time resolutions, from several seconds down to sub-ms scales. Using the dispersion measures in excess of the Galactic terms, we estimated the upper limits on the redshifts. Results: No convincing signal was found, and for each FRB we constrained the γ-ray isotropic-equivalent luminosity and the released energy as a function of emission timescale. For the nearest FRB source, the periodic repeater FRB 180916.J0158+65, we find Lγ, iso < 5.5 × 1047 erg s-1 over 1 s, whereas Lγ, iso < 1049 - 1051 erg s-1 for the bulk of FRBs. The same values scale up by a factor of ∼100 for a ms-long emission. Conclusions: Even on a timescale comparable with that of the radio pulse itself, no keV-MeV emission is observed. A systematic association with either long or short GRBs is ruled out with high confidence, except for sub-luminous events, as is the case for the core-collapse of massive stars (long) or binary neutron star mergers (short) viewed off axis. Only giant flares from extragalactic magnetars at least ten times more energetic than Galactic siblings are ruled out for the nearest FRB.
Aims: We aim to search for prompt γ-ray counterparts in the Insight-Hard X-ray Modulation Telescope (Insight-HXMT) data, taking advantage of the unique combination of the large effective area in the keV-MeV energy range, and of sub-ms time resolution. Methods: We selected 39 FRBs that were promptly visible from the High-Energy (HE) instrument aboard Insight-HXMT. After calculating the expected arrival times at the location of the spacecraft, we searched for a significant excess in both individual and cumulative time profiles over a wide range of time resolutions, from several seconds down to sub-ms scales. Using the dispersion measures in excess of the Galactic terms, we estimated the upper limits on the redshifts. Results: No convincing signal was found, and for each FRB we constrained the γ-ray isotropic-equivalent luminosity and the released energy as a function of emission timescale. For the nearest FRB source, the periodic repeater FRB 180916.J0158+65, we find Lγ, iso < 5.5 × 1047 erg s-1 over 1 s, whereas Lγ, iso < 1049 - 1051 erg s-1 for the bulk of FRBs. The same values scale up by a factor of ∼100 for a ms-long emission. Conclusions: Even on a timescale comparable with that of the radio pulse itself, no keV-MeV emission is observed. A systematic association with either long or short GRBs is ruled out with high confidence, except for sub-luminous events, as is the case for the core-collapse of massive stars (long) or binary neutron star mergers (short) viewed off axis. Only giant flares from extragalactic magnetars at least ten times more energetic than Galactic siblings are ruled out for the nearest FRB.
Volume
637
Start page
A69
Issn Identifier
0004-6361
Ads BibCode
2020A&A...637A..69G
Rights
open.access
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