RT Journal Article
T1 Detection of bridge emission above 50 GeV from the Crab pulsar 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 Satalecka, Konstanzja
A1 Scapin, Valeria
AB Context. The Crab pulsar is the only astronomical pulsed source detected at very high energy (VHE, E > 100 GeV) gamma rays. The emission mechanism of VHE pulsation is not yet fully understood, although several theoretical models have been proposed. Aims. In order to test new models, we measured the light curve and the spectra of the Crab pulsar with high precision by means of deep observations. Methods. We analyzed 135 h of selected MAGIC data taken between 2009 and 2013 in stereoscopic mode. In order to discuss the spectral shape in connection with lower energies, 5.5 years of Fermi-LAT data were also analyzed. Results. The known two pulses per period were detected with a significance of 8.0 sigma and 12.6 sigma. In addition, significant emission was found between the two pulses with 6.2 sigma. Conclusions. We discovered the bridge emission above 50 GeV between the two main pulses. This emission can not be explained with the existing theories. These data can be used for testing new theoretical models.
PB EDP Sciencies
SN 0004-6361
YR 2014
FD 2014-05
LK https://hdl.handle.net/20.500.14352/33639
UL https://hdl.handle.net/20.500.14352/33639
LA eng
NO © ESO. We would like to thank Felix Aharonian and Dmitry Khangulyan for useful discussions on the pulsar emission models. We would also like to thank the Instituto de Astrofísica de Canarias for the excellent working conditions at the Observatorio del Roque de losMuchachos in La Palma. The support of the German BMBF and MPG, the Italian INFN, the Swiss National Fund SNF, and the Spanish MINECO is gratefully acknowledged. This work was also supported by the CPAN CSD2007-00042 and MultiDark CSD2009-00064 projects of the Spanish Consolider-Ingenio 2010 programme, by grant DO02-353 of the Bulgarian NSF, by grant 127740 of the Academy of Finland, by the DFG Cluster of Excellence “Origin and Structure of the Universe”, by the DFG Collaborative Research Centers SFB823/C4 and SFB876/C3, by the Polish MNiSzW grant 745/N-HESS-MAGIC/2010/0, by the Croatian Science Foundation (HrZZ) Project 09/186 and by the Formosa Program between National Science Council in Taiwan and Consejo Superior de Investigaciones Cientificas in Spain administered through grant number NSC100-2923-M-007-001-MY3.
NO German BMBF
NO German MPG
NO Italian INFN
NO Swiss National Fund SNF
NO Spanish MINECO
NO Spanish Consolider-Ingenio 2010
NO Bulgarian NSF
NO Academy of Finland
NO DFG Cluster of Excellence “Origin and Structure of the Universe”
NO DFG Collaborative Research Centers
NO Polish MNiSzW
NO Croatian Science Foundation (HrZZ)
NO National Science Council in Taiwan
NO Consejo Superior de Investigaciones Cientificas in Spain
DS Docta Complutense
RD 10 abr 2025