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Observation of pulsed gamma-rays above 25 GeV from the Crab Pulsar with MAGIC

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dc.contributor.authorAntoranz Canales, Pedro
dc.contributor.authorBarrio Uña, Juan Abel
dc.contributor.authorContreras González, José Luis
dc.contributor.authorFonseca González, María Victoria
dc.contributor.authorMiranda Pantoja, José Miguel
dc.contributor.authorNieto Castaño, Daniel
dc.date.accessioned2023-06-20T10:37:24Z
dc.date.available2023-06-20T10:37:24Z
dc.date.issued2008-11-21
dc.description© Science. We thank the electronics division at the Max-Planck-Insitut, Munich, for their work in developing and producing the analog sum trigger system, especially O. Reimann, R. Maier, S. Tran, and T. Dettlaff. We also thank L. Stodolsky for comments. We acknowledge the Instituto de Astrofisica for providing all infrastructure on the Roque de los Muchachos in La Palma. The support of the German Bundesministerium fur Bildung, Wissenschaft, Forschung und Technologie and Max-Planck-Gesellschaft, the Italian INFN and INAF, the Swiss Schweizerische Nationalfonds, and Spanish Ministerio de Ciencia e Innovacion is acknowledged. This work was also supported by ETH research grant TH 34/043, by the Polish Ministertwo Nauki i Szkolnictwa Wyzszego grant N N203 390834, and by the Young Investigators Program of the Helmholtz Gemeinschaft.
dc.description.abstractOne fundamental question about pulsars concerns the mechanism of their pulsed electromagnetic emission. Measuring the high- end region of a pulsar's spectrum would shed light on this question. By developing a new electronic trigger, we lowered the threshold of the Major Atmospheric gamma-ray Imaging Cherenkov (MAGIC) telescope to 25 giga-electron volts. In this configuration, we detected pulsed gamma-rays from the Crab pulsar that were greater than 25 giga-electron volts, revealing a relatively high cutoff energy in the phase- averaged spectrum. This indicates that the emission occurs far out in the magnetosphere, hence excluding the polar- cap scenario as a possible explanation of our measurement. The high cutoff energy also challenges the slot- gap scenario.
dc.description.departmentDepto. de Estructura de la Materia, Física Térmica y Electrónica
dc.description.facultyFac. de Ciencias Físicas
dc.description.refereedTRUE
dc.description.sponsorshipGerman Bundesministerium fur Bildung, Wissenschaft, Forschung und Technologie
dc.description.sponsorshipMax-Planck-Gesellschaft
dc.description.sponsorshipItalian INFN and INAF
dc.description.sponsorshipSwiss Schweizerische Nationalfonds
dc.description.sponsorshipSpanish Ministerio de Ciencia e Innovacion
dc.description.sponsorshipETH
dc.description.sponsorshipPolish Ministertwo Nauki i Szkolnictwa Wyzszego
dc.description.sponsorshipYoung Investigators Program of the Helmholtz Gemeinschaft
dc.description.statuspub
dc.eprint.idhttps://eprints.ucm.es/id/eprint/23066
dc.identifier.doi10.1126/science.1164718
dc.identifier.issn0036-8075
dc.identifier.officialurlhttp://dx.doi.org/10.1126/science.1164718
dc.identifier.relatedurlhttp://www.sciencemag.org
dc.identifier.relatedurlhttp://arxiv.org/abs/0809.2998
dc.identifier.urihttps://hdl.handle.net/20.500.14352/50806
dc.issue.number5905
dc.journal.titleScience
dc.language.isoeng
dc.page.final1224
dc.page.initial1221
dc.publisherAmer Assoc Advancement Science
dc.relation.projectIDTH 34/043
dc.relation.projectIDN N203 390834
dc.rights.accessRightsopen access
dc.subject.cdu537
dc.subject.cdu539.1
dc.subject.keywordOuter Magnetosphere
dc.subject.keywordSlot Gaps
dc.subject.keywordEmission
dc.subject.keywordRadiation
dc.subject.keywordTEV
dc.subject.keywordTelescope
dc.subject.keywordSearch
dc.subject.keywordAcceleration
dc.subject.keywordNebula.
dc.subject.ucmElectrónica (Física)
dc.subject.ucmElectricidad
dc.subject.ucmFísica nuclear
dc.subject.unesco2202.03 Electricidad
dc.subject.unesco2207 Física Atómica y Nuclear
dc.titleObservation of pulsed gamma-rays above 25 GeV from the Crab Pulsar with MAGIC
dc.typejournal article
dc.volume.number322
dcterms.references1. M. A. Ruderman, P. G. Sutherland, Astrophys. J. 196, 51(1975). 2. J. K. Daugherty, A. K. Harding, Astrophys. J. 252, 337 (1982). 3. M. G. Baring, Adv. Space Res. 33, 552 (2004). 4. J. Arons, E. T. Scharlemann, Astrophys. J. 231, 854 (1979). 5. A.G.Muslimov, A. K.Harding, Astrophys. J. 606, 1143 (2004). 6. A. K. Harding, J. V. Stern, J. Dyks, F. Frackowiak, Astrophys. J. 680, 1378 (2008). 7. K. S. Cheng, C. Ho, M. Ruderman, Astrophys. J. 300, 500(1986). 8. K. Hirotani, arXiv:0809.1283, (2008). 9. A. P. S. Tang, J. Takata, J. Jia, K. S. Cheng, Astrophys. J. 676, 562 (2008). 10. g-rays induce particle air showers in the atmosphere that emit Cherenkov light. The detection of this light allows measuring the energy and the direction of the incident g-ray. 11. P. Chadwick et al., Astropart. Phys. 9, 131 (1998). 12. P. G. Edwards et al., Astron. Astrophys. 291, 468 (1994). 13. F. Aharonian et al., Astrophys. J. 614, 897 (2004). 14. M. de Naurois et al., Astrophys. J. 566, 343 (2002). 15. R. W. Lessard et al., Astrophys. J. 531, 942 (2000). 16. F. Aharonian et al., Astron. Astrophys. 466, 543 (2007). 17. L. Kuiper et al., Astron. Astrophys. 378, 918 (2001). 18. See the MAGIC telescope Web site; http://wwwmagic. mppmu.mpg.de. 19. A. N. Otte, thesis, Technical University, Munich (2007); available online at http://mediatum2.ub.tum.de/doc/ 620881/document.pdf. 20. J. Albert et al., Astrophys. J. 674, 1037 (2008). 21. The threshold of a Cherenkov telescope is usually defined as the peak in the energy distribution of triggered g-ray events for a g-ray source with an E−2.6 power-law photon energy spectrum. 22. A. G. Lyne, R. S. Pritchard, F. Smith, Mon. Not. R. Astron. Soc. 265, 1003 (1993). 23. R. W. Romani, Astrophys. J. 470, 469 (1996). 24. P. Goldreich, W. H. Julian, Astrophys. J. 157, 869 (1969). 25. Data provided by EGRET; ftp://legacy.gsfc.nasa.gov/compton/data/egret/. 26. F. Lucarelli et al., Nucl. Instr. Meth. A 589, 415 (2008). 27. A. K. Harding, private communication.Investigators Program of the Helmholtz Gemeinschaft.
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