2025A&A...700A..96A

Query : 2025A&A...700A..96A

2025A&A...700A..96A - Astronomy and Astrophysics, volume 700A96 (2025/8-1)

Testing the ubiquitous presence of very high energy emission in gamma-ray bursts with the MAGIC telescopes.

ABE S., ABHIR J., ABHISHEK A., ACCIARI V.A., AGUASCA-CABOT A., AGUDO I., ANIELLO T., ANSOLDI S., ANTONELLI L.A., ARBET ENGELS A., ARCARO C., ARNESEN T.T.H., ASANO K., BABIC A., BAKSHI C., BARRES DE ALMEIDA U., BARRIO J.A., BARRIOS-JIMENEZ L., BATKOVIC I., BAXTER J., BECERRA GONZALEZ J., BEDNAREK W., BERNARDINI E., BERNETE J., BERTI A., BESENRIEDER J., BIGONGIARI C., BILAND A., BLANCH O., BONNOLI G., BOSNJAK Z., BRONZINI E., BURELLI I., CAMPOY-ORDAZ A., CAROSI A., CAROSI R., CARRETERO-CASTRILLO M., CASTRO-TIRADO A.J., CERASOLE D., CERIBELLA G., CHAI Y., CIFUENTES A., CONTRERAS J.L., CORTINA J., COVINO S., D'AMICO G., DA VELA P., DAZZI F., DE ANGELIS A., DE LOTTO B., DE MENEZES R., DELFINO M., DELGADO J., DELGADO MENDEZ C., DI PIERRO F., DI TRIA R., DI VENERE L., DINESH A., DOMINIS PRESTER D., DONINI A., DORNER D., DORO M., EISENBERGER L., ELSAESSER D., ESCUDERO J., FARINA L., FATTORINI A., FOFFANO L., FONT L., FROSE S., FUKAMI S., FUKAZAWA Y., GARCIA LOPEZ R.J., GARCIA SOTO S., GARCZARCZYK M., GASPARYAN S., GAUG M., GIESBRECHT PAIVA J.G., GIGLIETTO N., GIORDANO F., GLIWNY P., GODINOVIC N., GRADETZKE T., GRAU R., GREEN D., GREEN J.G., GUNTHER P., HADASCH D., HAHN A., HASSAN T., HECKMANN L., HERRERA LLORENTE J., HRUPEC D., IMAZAWA R., INOUE S., ISRAYELYAN D., JAHANVI J., JIMENEZ MARTINEZ I., JIMENEZ QUILES J., JORMANAINEN J., KANKKUNEN S., KAYANOKI T., KONRAD J., KOUCH P.M., KUBO H., KUSHIDA J., LAINEZ M., LAMASTRA A., LINDFORS E., LOMBARDI S., LONGO F., LOPEZ-COTO R., LOPEZ-MOYA M., LOPEZ-ORAMAS A., LOPORCHIO S., LULIC L., LYARD E., MAJUMDAR P., MAKARIEV M., MALLAMACI M., MANEVA G., MANGANARO M., MANGANO S., MANNHEIM K., MARCHESI S., MARIOTTI M., MARTINEZ M., MARUSEVEC P., MAS-AGUILAR A., MAZIN D., MENCHIARI S., MENDEZ GALLEGO J., MENON S., MICELI D., MIRANDA J.M., MIRZOYAN R., MOLERO GONZALEZ M., MOLINA E., MONDAL H.A., MORALEJO A., MORETTI E., NAKAMORI T., NANCI C., NAVA L., NEUSTROEV V., NICKEL L., NIEVAS ROSILLO M., NIGRO C., NIKOLIC L., NILSSON K., NISHIJIMA K., NODA K., NOZAKI S., OKUMURA A., OTERO-SANTOS J., PAIANO S., PANEQUE D., PAOLETTI R., PAREDES J.M., PERESANO M., PERSIC M., PIHET M., PIROLA G., PODOBNIK F., PRADA MORONI P.G., PRANDINI E., RIBO M., RICO J., RIGHI C., SAHAKYAN N., SAITO T., SATURNI F.G., SCHMITZ K., SCHMUCKERMAIER F., SCIACCALUGA A., SILVESTRI G., SIMONGINI A., SITAREK J., SLIUSAR V., SOBCZYNSKA D., STAMERRA A., STRISKOVIC J., STROM D., STRZYS M., SUDA Y., TAJIMA H., TAKAHASHI M., TAKEISHI R., TEMNIKOV P., TERAUCHI K., TERZIC T., TESHIMA M., TUTONE A., UBACH S., VAN SCHERPENBERG J., VAZQUEZ ACOSTA M., VENTURA S., VERNA G., VIALE I., VIGLIANO A., VIGORITO C.F., VISENTIN E., VITALE V., VOVK I., WALTER R., WERSIG F., WILL M., YAMAMOTO T. and YEUNG P.K.H.

Abstract (from CDS):

Gamma-ray bursts (GRBs) are the most powerful transient objects in the Universe, and they are a primary target for the MAGIC Collaboration. Recognizing the challenges of observing these elusive objects with Imaging Atmospheric Cherenkov Telescopes (IACTs), we implemented a dedicated observational strategy that included an automated procedure for rapid re-pointing to transient sources. Since 2013, this automated procedure has enabled MAGIC to observe GRBs at a rate of approximately ten per year, which led to the successful detection of two GRBs at very high energies (VHE; E > 100 GeV). We present a comprehensive analysis of 42 non-detected GRBs (4 short GRBs) observed by MAGIC from 2013 to 2019. We derived upper limits (ULs) on the observed energy flux as well as on the intrinsic energy flux corrected for absorption by the extragalactic background light (EBL) from the MAGIC observations in selected energy and time intervals. We conducted a comprehensive study of their properties to investigate the reasons for these non-detections, including the possible peculiar properties of TeV-detected GRBs. We find that strong EBL absorption significantly hinders TeV detection for the majority of GRBs in our sample. For a subset of 6 GRBs with redshift z < 2, we compared the UL on the intrinsic flux in the VHE domain with the simultaneous X-ray flux, which is observed to be at the same level in the current population of TeV-detected GRBs. Based on these inferred MAGIC ULs, we conclude that a VHE component with a luminosity comparable to the simultaneously observed X-ray luminosity cannot be ruled out for this sample.

Abstract Copyright: © The Authors 2025

Journal keyword(s): radiation mechanisms: non-thermal - gamma-ray burst: general - gamma rays: general

Simbad objects: 47

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Number of rows : 47
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 GRB 180720B gB 00 02 06.99 -02 55 07.8           ~ 215 0
2 GRB 140930B gB 00 25 23.40 +24 17 41.7           ~ 52 0
3 GRB 201216C gB 01 05 28.88 +16 30 58.0           ~ 89 0
4 GRB 190106A gB 01 59 31.23 +23 50 43.8           ~ 66 0
5 GRB 191004A gB 02 06 40.42 -36 56 04.8           ~ 16 0
6 GRB 171020A gB 02 36 59.62 +15 12 14.6           ~ 28 0
7 GRB 150819A gB 02 49 19.94 +09 48 27.1           ~ 20 0
8 GRB 141026A gB 02 56 20.29 +26 55 42.4           ~ 60 0
9 SN 2019oyw SN* 02 58 10.510 -08 57 27.20           ~ 218 0
10 GRB 190114C gB 03 38 01.18 -26 56 47.8           ~ 343 0
11 GRB 151118A gB 03 48 41.16 +65 54 06.0           ~ 22 0
12 Fermi bn161229878 gB 05 24 +06.3           ~ 10 0
13 Fermi bn130903033 gB 05 28 31.23 -00 07 36.0           ~ 17 0
14 M 1 SNR 05 34 31.8 +22 01 03           ~ 6516 1
15 GRB 151215A gB 06 14 20.20 +35 30 58.3           ~ 47 0
16 GRB 150213A gB 06 21 -04.8           ~ 15 0
17 GRB 160310A gB 06 35 17.33 -07 12 56.0           ~ 23 0
18 GRB 140430A gB 06 51 44.58 +23 01 25.5           ~ 81 0
19 Fermi bn170921168 gB 08 49 30.0 +57 03 25           ~ 9 0
20 Fermi bn130502743 gB 09 14 16.53 -00 07 24.1           ~ 38 0
21 GRB 160504A gB 11 20 17.33 +56 00 05.4           ~ 20 0
22 SN 2013cq SN* 11 32 32.84 +27 41 56.2           SNIc 613 1
23 GRB 160313A gB 12 15 11.19 +57 17 01.0           ~ 22 0
24 GRB 150428A gB 12 34 09.22 +06 57 13.2           ~ 23 0
25 Fermi bn141220252 gB 13 00 15.70 +32 08 47.2           ~ 81 0
26 GRB 180512A gB 13 27 45.12 +21 24 12.4           ~ 18 0
27 GRB 160119A gB 14 07 41.27 +20 27 39.3           ~ 26 0
28 GRB 160910A gB 14 45 46.04 +39 04 01.3           ~ 45 0
29 GRB 180715A gB 15 40 20.50 -00 53 57.6           ~ 24 0
30 Fermi bn170728961 G 15 51 55.5290 +70 07 22.038           ~ 54 0
31 GRB 130606A gB 16 37 35.12 +29 47 46.4           ~ 185 0
32 GRB 160927A gB 17 04 58.19 +17 19 55.3           ~ 34 0
33 Fermi bn130612141 gB 17 19 10.63 +16 43 11.8           ~ 89 0
34 GRB 180720C gB 17 42 32.63 -26 37 45.1           ~ 15 0
35 GRB 130504A gB 18 09 49.49 -16 18 48.6           ~ 26 0
36 GRB 180904A gB 18 16 59.94 +46 37 46.9           ~ 20 0
37 Fermi bn160821937 gB 18 39 54.550 +62 23 30.35           ~ 190 0
38 GRB 221009A gB 19 13 03.85 +19 46 22.7           ~ 433 0
39 GRB 150428B gB 19 30 33.46 +04 07 31.8           ~ 23 0
40 Fermi bn140709051 gB 20 18 38.96 +51 13 29.9           ~ 43 0
41 GRB 160625B gB 20 34 23.67 +06 55 11.1           ~ 235 0
42 Fermi bn160509374 gB 20 47 00.90 +76 06 30.1           ~ 141 0
43 GRB 160623A gB 21 01 11.54 +42 13 15.5           ~ 73 0
44 Fermi bn171210493 gB 22 21 09.6 +24 26 24           ~ 20 0
45 GRB 131030A gB 23 00 16.14 -05 22 05.2           ~ 126 0
46 GRB 181225A gB 23 12.3 -09 29           ~ 15 0
47 GRB 130701A gB 23 48 55.05 +36 06 01.2           ~ 81 0

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