RT Journal Article
T1 Detection of very high energy gamma-ray emission from the gravitationally lensed blazar QSO B0218+357 with the MAGIC telescopes
A1 Antoranz Canales, Pedro
A1 Barrio Uña, Juan Abel
A1 Contreras González, José Luis
A1 Fonseca González, María Victoria
A1 López Moya, Marcos
A1 Miranda Pantoja, José Miguel
A1 Nievas Rosillo, Mireia
AB Context. QSO B0218+357 is a gravitationally lensed blazar located at a redshift of 0.944. The gravitational lensing splits the emitted radiation into two components that are spatially indistinguishable by gamma-ray instruments, but separated by a 10–12 day delay. In July 2014, QSO B0218+357 experienced a violent flare observed by the Fermi-LAT and followed by the MAGIC telescopes.Aims. The spectral energy distribution of QSO B0218+357 can give information on the energetics of z ∼ 1 very high energy gamma-ray sources. Moreover the gamma-ray emission can also be used as a probe of the extragalactic background light at z ∼ 1.Methods. MAGIC performed observations of QSO B0218+357 during the expected arrival time of the delayed component of the emission. The MAGIC and Fermi-LAT observations were accompanied by quasi-simultaneous optical data from the KVA telescope and X-ray observations by Swift-XRT. We construct a multiwavelength spectral energy distribution of QSO B0218+357 and use it to model the source. The GeV and sub-TeV data obtained by Fermi-LAT and MAGIC are used to set constraints on the extragalactic background light.Results. Very high energy gamma-ray emission was detected from the direction of QSO B0218+357 by the MAGIC telescopes during the expected time of arrival of the trailing component of the flare, making it the farthest very high energy gamma-ray source detected to date. The observed emission spans the energy range from 65 to 175 GeV. The combined MAGIC and Fermi-LAT spectral energy distribution of QSO B0218+357 is consistent with current extragalactic background light models. The broadband emission can be modeled in the framework of a two-zone external Compton scenario, where the GeV emission comes from an emission region in the jet, located outside the broad line region.
PB EDP Sciencies
SN 1432-0746
YR 2016
FD 2016-11
LK https://hdl.handle.net/20.500.14352/17748
UL https://hdl.handle.net/20.500.14352/17748
LA eng
NO © ESO, 2016. Artículo firmado por 53 autores.  We 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 (FPA2012-39502), and the Japanese JSPS and MEXT is gratefully acknowledged. This work was also supported by the Centro de Excelencia Severo Ochoa SEV-2012-0234, CPAN CSD2007-00042, and MultiDark CSD2009-00064 projects of the Spanish Consolider-Ingenio 2010 programme, by grant 268740 of the Academy of Finland, by the Croatian Science Foundation (HrZZ) Project 09/176 and the University of Rijeka Project 13.12.1.3.02, by the DFG Collaborative Research Centers SFB823/C4 and SFB876/C3, and by the Polish MNiSzW grant 745/N-HESS-MAGIC/2010/0. The Fermi LAT Collaboration acknowledges generous ongoing support from a number of agencies and institutes that have supported both the development and the operation of the LAT as well as scientific data analysis. These include the National Aeronautics and Space Administration and the Department of Energy in the United States, the Commissariat à l’Énergie Atomique and the Centre National de la Recherche Scientifique/Institut National de Physique Nucléaire et de Physique des Particules in France, the Agenzia Spaziale Italiana and the Istituto Nazionale di Fisica Nucleare in Italy, the Ministry of Education, Culture, Sports, Science and Technology (MEXT), High Energy Accelerator Research Organization (KEK) and Japan Aerospace Exploration Agency (JAXA) in Japan, and the K. A. Wallenberg Foundation, the Swedish Research Council and the Swedish National Space Board in Sweden. Additional support for science analysis during the operations phase is gratefully acknowledged from the Istituto Nazionale di Astrofisica in Italy and the Centre National d’Études Spatiales in France.
NO Ministerio de Economía y Competitividad (MINECO)
NO German BMBF
NO German MPG
NO Italian INFN
NO Italian INAF
NO Swiss National Fund SNF
NO Japanese JSPS
NO Japanese MEXT
NO Centro de Excelencia Severo Ochoa
NO Spanish Consolider-Ingenio 2010 programme
NO Academy of Finland
NO Croatian Science Foundation (HrZZ)
NO University of Rijeka
NO DFG Collaborative Research Centers
NO Polish MNiSzW
NO National Aeronautics and Space Administration in the United States
NO Department of Energy in the United States
NO Commissariat à l’Énergie Atomique in France
NO Centre National de la Recherche Scientifique/Institut National de Physique Nucléaire et de Physique des Particules in France
NO Agenzia Spaziale Italiana
NO Istituto Nazionale di Fisica Nucleare in Italy
NO Ministry of Education, Culture, Sports, Science and Technology (MEXT)
NO High Energy Accelerator Research Organization (KEK) in Japan
NO Japan Aerospace Exploration Agency (JAXA) in Japan
NO K. A. Wallenberg Foundation in Sweden
NO Swedish Research Council in Sweden
NO Swedish National Space Board in Sweden
NO Istituto Nazionale di Astrofisica in Italy
NO Centre National d’Études Spatiales in France
DS Docta Complutense
RD 5 abr 2025