2019MNRAS.482..184A

Query : 2019MNRAS.482..184A

2019MNRAS.482..184A - Mon. Not. R. Astron. Soc., 482, 184-193 (2019/January-1)

The search for high-energy neutrinos coincident with fast radio bursts with the ANTARES neutrino telescope.

ALBERT A., ANDRE M., ANGHINOLFI M., ANTON G., ARDID M., AUBERT J.-J., AUBLIN J., AVGITAS T., BARET B., BARRIOS-MARTI J., BASA S., BELHORMA B., BERTIN V., BIAGI S., BORMUTH R., BOUMAAZA J., BOURRET S., BOUWHUIS M.C., BRANZAS H., BRUIJN R., BRUNNER J., BUSTO J., CAPONE A., CARAMETE L., CARR J., CELLI S., CHABAB M., CHERKAOUI EL MOURSLI R., CHIARUSI T., CIRCELLA M., COELHO J.A.B., COLEIRO A., COLOMER M., CONIGLIONE R., COSTANTINI H., COYLE P., CREUSOT A., DIAZ A.F., DESCHAMPS A., DISTEFANO C., DI PALMA I., DOMI A., DONZAUD C., DORNIC D., DROUHIN D., EBERL T., EL BOJADDAINI I., EL KHAYATI N., ELSASSER D., ENZENHOFER A., ETTAHIRI A., FASSI F., FELIS I., FERMANI P., FERRARA G., FUSCO L., GAY P., GLOTIN H., GREGOIRE T., GRACIA-RUIZ R., GRAF K., HALLMANN S., VAN HAREN H., HEIJBOER A.J., HELLO Y., HERNANDEZ-REY J.J., HOSSL J., HOFESTADT J., ILLUMINATI G., JAMES C.W., DE JONG M., JONGEN M., KADLER M., KALEKIN O., KATZ U., KOUCHNER A., KRETER M., KREYKENBOHM I., KULIKOVSKIY V., LACHAUD C., LAHMANN R., LEFEVRE D., LEONORA E., LEVI G., LOTZE M., LOUCATOS S., MARCELIN M., MARGIOTTA A., MARINELLI A., MARTINEZ-MORA J.A., MELE R., MELIS K., MIGLIOZZI P., MOUSSA A., NAVAS S., NEZRI E., NUNEZ A., ORGANOKOV M., PAVALAS G.E., PELLEGRINO C., PIATTELLI P., POPA V., PRADIER T., QUINN L., RACCA C., RANDAZZO N., RICCOBENE G., SANCHEZ-LOSA A., SALDANA M., SALVADORI I., SAMTLEBEN D.F.E., SANGUINETI M., SAPIENZA P., SCHUSSLER F., SPURIO M., STOLARCZYK T., TAIUTI M., TAYALATI Y., TROVATO A., TURPIN D., VALLAGE B., VAN ELEWYCK V., VERSARI F., VIVOLO D., WILMS J., ZABOROV D., ZORNOZA J.D. and ZUNIGA J.

Abstract (from CDS):

In the past decade, a new class of bright transient radio sources with millisecond duration has been discovered. The origin of these so-called fast radio bursts (FRBs) is still a mystery, despite the growing observational efforts made by various multiwavelength and multimessenger facilities. To date, many models have been proposed to explain FRBs, but neither the progenitors nor the radiative and the particle acceleration processes at work have been clearly identified. In this paper, we assess whether hadronic processes may occur in the vicinity of the FRB source. If they do, FRBs may contribute to the high-energy cosmic-ray and neutrino fluxes. A search for these hadronic signatures was carried out using the ANTARES neutrino telescope. The analysis consists in looking for high-energy neutrinos, in the TeV-PeV regime, that are spatially and temporally coincident with the detected FRBs. Most of the FRBs discovered in the period 2013-2017 were in the field of view of the ANTARES detector, which is sensitive mostly to events originating from the Southern hemisphere. From this period, 12 FRBs were selected and no coincident neutrino candidate was observed. Upper limits on the per-burst neutrino fluence were derived using a power-law spectrum, dN/ dEν_∝E_ν–γ^, for the incoming neutrino flux, assuming spectral indexes γ = 1.0, 2.0, 2.5. Finally, the neutrino energy was constrained by computing the total energy radiated in neutrinos, assuming different distances for the FRBs. Constraints on the neutrino fluence and on the energy released were derived from the associated null results.

Abstract Copyright: © 2018 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society

Journal keyword(s): acceleration of particles - neutrinos - astroparticle physics - radio continuum: transients - methods: data analysis

Simbad objects: 18

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Number of rows : 18
N Identifier Otype ICRS (J2000)
RA 		ICRS (J2000)
DEC 		Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2026 		#notes
1 NAME Magellanic Clouds GrG 03 00 -71.0           ~ 7988 0
2 PMN J0509+0541 BLL 05 09 25.9644373872 +05 41 35.333820420 15.32 14.95 14.78 15.12   ~ 589 2
3 FRB 20181119D rB 05 31 58.6980 +33 08 52.588           ~ 933 0
4 FRB 131104 rB 06 44 10.4 -51 16 40           ~ 83 0
5 FRB 150418 rB 07 16 30.9 -19 02 24           ~ 120 0
6 FRB 160608 rB 07 36 42.0 -40 47 52           ~ 17 0
7 FRB 160317 rB 07 53 47.0 -29 36 31           ~ 22 0
8 FRB 160410 rB 08 41 25.0 +06 05 05           ~ 18 0
9 FRB 151230 rB 09 40 50.0 -03 27 05           ~ 31 0
10 FRB 150610 rB 10 44 26.0 -40 05 23           ~ 19 0
11 FRB 170107 rB 11 23 10 -05 01.0           ~ 27 0
12 GrW 170817 GWE 13 09 48.0850 -23 22 53.343           ~ 2683 0
13 PSR J1808-2024 Psr 18 08 39.32 -20 24 40.1           ~ 1316 2
14 FRB 150215 rB 18 17 27.0 -04 54 15           ~ 42 0
15 FRB 151206 rB 19 21 25.0 -04 07 54           ~ 18 0
16 FRB 140514 rB 22 34 06.20 -12 18 46.5           ~ 80 0
17 FRB 20160102A rB 22 38 49.0 -30 10 50           ~ 41 0
18 FRB 150807 rB 22 41 33.75 -53 05 39.9           ~ 66 0

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