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Por favor, use este identificador para citar o enlazar a este item: http://hdl.handle.net/10261/260783
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dc.contributor.authorAcciari, Victor-
dc.contributor.authorCerruti, Matteo-
dc.contributor.authorMolina, E.-
dc.contributor.authorParedes, Josep M.-
dc.contributor.authorRibó, Marc-
dc.contributor.authorTorres-Albà, N.-
dc.contributor.authorFont, L.-
dc.contributor.authorGaug, Markus-
dc.contributor.authorMaggio, C.-
dc.contributor.authorMoreno, V.-
dc.contributor.authorNava, Lara-
dc.contributor.authorMAGIC Collaboration-
dc.date.accessioned2022-02-14T12:40:03Z-
dc.date.available2022-02-14T12:40:03Z-
dc.date.issued2021-02-16-
dc.identifierdoi: 10.3847/1538-4357/abd249-
dc.identifierissn: 1538-4357-
dc.identifier.citationAstrophysical Journal 908: 90 (2021)-
dc.identifier.urihttp://hdl.handle.net/10261/260783-
dc.descriptionAcciari, A. V., et al.-
dc.description.abstractThe coincident detection of GW170817 in gravitational waves and electromagnetic radiation spanning the radio to MeV gamma-ray bands provided the first direct evidence that short gamma-ray bursts (GRBs) can originate from binary neutron star (BNS) mergers. On the other hand, the properties of short GRBs in high-energy gamma-rays are still poorly constrained, with only ∼20 events detected in the GeV band, and none in the TeV band. GRB 160821B is one of the nearest short GRBs known at z = 0.162. Recent analyses of the multiwavelength observational data of its afterglow emission revealed an optical-infrared kilonova component, characteristic of heavy-element nucleosynthesis in a BNS merger. Aiming to better clarify the nature of short GRBs, this burst was automatically followed up with the MAGIC telescopes, starting from 24 s after the burst trigger. Evidence of a gamma-ray signal is found above ∼0.5 TeV at a significance of ∼ 3σ during observations that lasted until 4 hr after the burst. Assuming that the observed excess events correspond to gamma-ray emission from GRB 160821B, in conjunction with data at other wavelengths, we investigate its origin in the framework of GRB afterglow models. The simplest interpretation with one-zone models of synchrotron-self-Compton emission from the external forward shock has difficulty accounting for the putative TeV flux. Alternative scenarios are discussed where the TeV emission can be relatively enhanced. The role of future GeV-TeV observations of short GRBs in advancing our understanding of BNS mergers and related topics is briefly addressed.-
dc.description.sponsorshipWe would like to thank the Instituto de Astrofísica de Canarias for the excellent working conditions at the Observatorio del Roque de los Muchachos in La Palma. The financial support of the German BMBF and MPG; the Italian INFN and INAF; the Swiss National Fund SNF; the ERDF under the Spanish MINECO (FPA2017-87859-P, FPA2017-85668-P, FPA2017- 82729-C6-2-R, FPA2017-82729-C6-6-R, FPA2017-82729-C6-5- R, AYA2015-71042-P, AYA2016-76012-C3-1-P, ESP2017- 87055-C2-2-P, FPA2017-90566-REDC); the Indian Department of Atomic Energy; the Japanese ICRR, the University of Tokyo, JSPS, and MEXT; the Bulgarian Ministry of Education and Science, National RI Roadmap Project DO1-268/16.12.2019 and the Academy of Finland grant No. 320045 is gratefully acknowledged. This work was also supported by the Spanish Centro de Excelencia “Severo Ochoa” SEV-2016-0588, SEV2015-0548 and SEV-2012-0234, the Unidad de Excelencia “María de Maeztu” MDM-2014-0369 and the “la Caixa” Foundation (fellowship LCF/BQ/PI18/11630012), by the Croatian Science Foundation (HrZZ) Project IP-2016-06-9782 and the University of Rijeka Project 13.12.1.3.02, by the DFG Collaborative Research Centers SFB823/C4 and SFB876/C3, the Polish National Research Centre grant UMO-2016/22/M/ST9/ 00382 and by the Brazilian MCTIC, CNPq and FAPERJ. K.N. is thankful for the support by Marie Skłodowska-Curie actions (H2020-MSCA-COFUND-2014, Project P-Sphere GA 665919), and JSPS KAKENHI grant No. JP20KK0067 from MEXT, Japan. L.N. acknowledges funding from the European Union’s Horizon 2020 research and innovation program under the Marie Skłodowska-Curie grant agreement No. 664931. S.I. is supported by JSPS KAKENHI grant No. JP17K05460 from MEXT, Japan, and the RIKEN iTHEMS program.-
dc.languageeng-
dc.publisherIOP Publishing-
dc.relationinfo:eu-repo/grantAgreement/AEI/Plan Estatal de Investigación Científica y Técnica y de Innovación 2013-2016/FPA2017-87859-P/ES/OPERACION Y EXPLOTACION CIENTIFICA DE LOS TELESCOPIOS MAGIC/-
dc.relationinfo:eu-repo/grantAgreement/AEI/Plan Estatal de Investigación Científica y Técnica y de Innovación 2013-2016/FPA2017-85668-P/ES/ASTROFISICA DE ALTAS ENERGIAS CON MAGIC/-
dc.relationinfo:eu-repo/grantAgreement/AEI/Plan Estatal de Investigación Científica y Técnica y de Innovación 2013-2016/FPA2017-82729-C6-2-R/ES/CONTRIBUCION DEL ICCUB A LA PUESTA EN MARCHA Y PRIMERA CIENCIA DEL OBSERVATORIO CTA-N/-
dc.relationinfo:eu-repo/grantAgreement/AEI/Plan Estatal de Investigación Científica y Técnica y de Innovación 2013-2016/FPA2017-82729-C6-6-R/ES/CONTRIBUCION DEL CIEMAT A LA PUESTA EN MARCHA Y PRIMERA CIENCIA DEL OBSERVATORIO CTA-N/-
dc.relationinfo:eu-repo/grantAgreement/AEI/Plan Estatal de Investigación Científica y Técnica y de Innovación 2013-2016/FPA2017-82729-C6-5-R/ES/UAB&CERES-IEEC CONTRIBUTION TO THE COMMISSIONING AND FIRST SCIENCE OF THE CTA-NORTH OBSERVATORY/-
dc.relationinfo:eu-repo/grantAgreement/MINECO//AYA2015-71042-P/ES/ESTUDIOS SOBRE LA INTERACCION PLASMA-CAMPO MAGNETICO EN ESCENARIOS ASTROFISICOS EXTREMOS/-
dc.relationinfo:eu-repo/grantAgreement/AEI/Plan Estatal de Investigación Científica y Técnica y de Innovación 2013-2016/ESP2017-87055-C2-2-P/ES/PARTICIPACION DEL IAC EN EL EXPERIMENTO AMS/-
dc.relation.isversionofPublisher's version-
dc.rightsopenAccess-
dc.subjectGamma ray bursts-
dc.titleMAGIC Observations of the Nearby Short Gamma-Ray Burst GRB 160821B-
dc.typeartículo-
dc.identifier.doi10.3847/1538-4357/abd249-
dc.relation.publisherversionhttp://doi.org/10.3847/1538-4357/abd249-
dc.date.updated2022-02-14T12:40:03Z-
dc.contributor.funderGerman Research Foundation-
dc.contributor.funderIstituto Nazionale di Fisica Nucleare-
dc.contributor.funderIstituto Nazionale di Astrofisica-
dc.contributor.funderSwiss National Science Foundation-
dc.contributor.funderMinisterio de Economía y Competitividad (España)-
dc.contributor.funderDepartment of Atomic Energy (India)-
dc.contributor.funderUniversity of Tokyo-
dc.contributor.funderJapan Society for the Promotion of Science-
dc.contributor.funderMinistry of Education, Culture, Sports, Science and Technology (Japan)-
dc.contributor.funderAcademy of Finland-
dc.contributor.funderPolish National Agency for Academic Exchange-
dc.contributor.funderJapan Society for the Promotion of Science-
dc.relation.csicSí-
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dc.identifier.funderhttp://dx.doi.org/10.13039/501100005184es_ES
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dc.identifier.funderhttp://dx.doi.org/10.13039/501100004721es_ES
dc.identifier.funderhttp://dx.doi.org/10.13039/501100003329es_ES
dc.identifier.funderhttp://dx.doi.org/10.13039/501100001502es_ES
dc.type.coarhttp://purl.org/coar/resource_type/c_6501es_ES
item.grantfulltextopen-
item.fulltextWith Fulltext-
item.openairecristypehttp://purl.org/coar/resource_type/c_18cf-
item.cerifentitytypePublications-
item.openairetypeartículo-
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