2020A&A...637A..69G

Query : 2020A&A...637A..69G

2020A&A...637A..69G - Astronomy and Astrophysics, volume 637A69-69 (2020/5-1)

A search for prompt γ-ray counterparts to fast radio bursts in the Insight-HXMT data.

GUIDORZI C., MARONGIU M., MARTONE R., NICASTRO L., XIONG S.L., LIAO J.Y., LI G., ZHANG S.N., AMATI L., FRONTERA F., ORLANDINI M., ROSATI P., VIRGILLI E., ZHANG S., BU Q.C., CAI C., CAO X.L., CHANG Z., CHEN G., CHEN L., CHEN T.X., CHEN Y.B., CHEN Y.P., CUI W., CUI W.W., DENG J.K., DONG Y.W., DU Y.Y., FU M.X., GAO G.H., GAO H., GAO M., GE M.Y., GU Y.D., GUAN J., GUO C.C., HAN D.W., HUANG Y., HUO J., JIA S.M., JIANG L.H., JIANG W.C., JIN J., JIN Y.J., KONG L.D., LI B., LI C.K., LI M.S., LI T.P., LI W., LI X., LI X.B., LI X.F., LI Y.G., LI Z.W., LIANG X.H., LIU B.S., LIU C.Z., LIU G.Q., LIU H.W., LIU X.J., LIU Y.N., LU B., LU F.J., LU X.F., LUO Q., LUO T., MA R.C., MA X., MENG B., NANG Y., NIE J.Y., OU G., QU J.L., SAI N., SHANG R.C., SONG L.M., SONG X.Y., SUN L., TAN Y., TAO L., TUO Y.L., WANG C., WANG G.F., WANG J., WANG W.S., WANG Y.S., WEN X.Y., WU B.Y., WU B.B., WU M., XIAO G.C., XIAO S., XU Y.P., YANG J.W., YANG S., YANG Y.J., YI Q.B., YIN Q.Q., YOU Y., ZHANG A.M., ZHANG C.M., ZHANG F., ZHANG H.M., ZHANG J., ZHANG T., ZHANG W.C., ZHANG W., ZHANG W.Z., ZHANG Y., ZHANG Y.F., ZHANG Y.J., ZHANG Y., ZHANG Z., ZHANG Z., ZHANG Z.L., ZHANG H.S., ZHANG X.F., ZHENG S.J., ZHOU D.K., ZHOU J.F., ZHU Y.X., ZHU Y. and ZHUANG R.L.

Abstract (from CDS):

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 L_γ,iso< 5.5x10⁴⁷erg/s over 1s, whereas L_γ,iso<10⁴⁹-10⁵¹erg/s 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.

Abstract Copyright: © ESO 2020

Journal keyword(s): radiation mechanisms: non-thermal - radio continuum: stars - gamma-ray burst: general

Simbad objects: 43

Full paper

View the references in ADS

Number of rows : 43

N	Identifier	Otype	ICRS (J2000) RA	ICRS (J2000) DEC	Mag B	Sp type	#ref 1850 - 2026	#notes
1	FRB 190806	rB	00 02 21.38	-07 34 54.6		~	9	0
2	FRB 20180916B	rB	01 58 00.750	+65 43 00.30		~	457	0
3	FRB 171216	rB	03 28.0	-57 04		~	14	0
4	FRB 180119	rB	03 29.3	-12 44		~	16	0
5	FRB 171116	rB	03 31.0	-17 14		~	16	0
6	FRB 171213	rB	03 39.0	-10 56		~	18	0
7	NAME FRB 180730.J0353+87	rB	03 49 33.6000	+87 11 24.000		~	12	0
8	FRB 20181119D	rB	05 31 58.6980	+33 08 52.588		~	933	0
9	M 1	SNR	05 34 31.8	+22 01 03		~	6516	1
10	NAME FRB 180729.J0558+56	rB	05 59 43.2000	+56 30 00.000		~	13	0
11	FRB 181228	rB	06 09 23.64	-45 58 02.4		~	16	0
12	FRB 180301	rB	06 12 43.40	+04 33 44.8		~	125	0
13	FRB 180528	rB	06 38 48.7	-49 53 59		~	9	0
14	NAME FRB 180810.J0646+34	rB	06 45 52.8000	+34 51 36.000		~	8	0
15	FRB 180430	rB	06 51.0	-09 57		~	10	0
16	NAME FRB 190209.J0937+77	rB	09 37 16.8000	+77 40 12.000		~	14	0
17	NAME FRB 181030.J1054+73	rB	10 33 24.0000	+73 47 24.000		~	79	0
18	FRB 171004	rB	11 57.6	-11 54		~	15	0
19	NAME FRB 180810.J1159+83	rB	12 01 38.4000	+83 08 24.000		~	13	0
20	FRB 190714	rB	12 15 55.1	-13 01 16		~	64	0
21	FRB 171003	rB	12 29.5	-14 07		~	15	0
22	NAME FRB 181119.J12+65	rB	12 41 52.0	+65 07 02		~	26	0
23	NAME FRB 190116.J1249+27	rB	12 49 08.0	+27 08 02		~	25	0
24	GrW 170817	GWE	13 09 48.0850	-23 22 53.343		~	2683	0
25	FRB 190523	rB	13 48 15.6	+72 28 11		~	109	0
26	FRB 20180128A	rB	13 56.0	-06 43		~	15	0
27	FRB 180525	rB	14 40.0	-02 12		~	14	0
28	NAME FRB 180817.J1533+42	rB	15 32 48.0000	+42 12 00.000		~	14	0
29	FRB 171209	rB	15 50 25.0	-46 10 20		~	27	0
30	FRB 180714	rB	17 46 12.0	-11 45 47		~	19	0
31	PSR J1808-2024	Psr	18 08 39.32	-20 24 40.1		~	1316	2
32	SN 1998bw	SN*	19 35 03.17	-52 50 46.1	14.09	SNIc	1928	2
33	FRB 180311	rB	21 31 33.42	-57 44 26.7		~	24	0
34	FRB 180924	rB	21 44 25.255	-40 54 00.10		~	140	0
35	FRB 180131	rB	21 49.9	-40 41		~	14	0
36	FRB 180110	rB	21 53.0	-35 27		~	21	0
37	FRB 20190711A	rB	21 57 40.7	-80 21 29		~	114	0
38	FRB 170906	rB	21 59.8	-19 57		~	16	0
39	FRB 181017	rB	22 05 54.820	-08 50 34.22		~	15	0
40	FRB 171019	rB	22 17.5	-08 40		~	52	0
41	HIDDEN NAME FRB 180128.2	rB	22 22.0	-60 15		~	15	0
42	FRB 170712	rB	22 36.0	-60 57		~	15	0
43	FRB 180515	rB	23 13 12.0	-42 14 46		~	8	0

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