Observations of the Crab Pulsar between 25 and 100 GeV with the MAGIC I Telescope

dc.contributor.authorAleksic, J.
dc.contributor.authorAlvarez, E. A.
dc.contributor.authorAntonelli, L. A.
dc.contributor.authorAntoranz, P.
dc.contributor.authorAsensio, M.
dc.contributor.authorBackes, M.
dc.contributor.authorBarrio, J. A.
dc.contributor.authorBastieri, D.
dc.contributor.authorBecerra González, J.
dc.contributor.authorBednarek, W.
dc.contributor.authorBerdyugin, A.
dc.contributor.authorZabalza, V.
dc.contributor.authorFerenc, D.
dc.contributor.authorZandanel, F.
dc.contributor.authorZanin, R.
dc.contributor.authorBoller, A.
dc.contributor.authorBonnoli, G.
dc.contributor.authorBorla Tridon, D.
dc.contributor.authorBraun, I.
dc.contributor.authorBretz, T.
dc.contributor.authorCañellas, A.
dc.contributor.authorLombardi, S.
dc.contributor.authorCarmona, E.
dc.contributor.authorCarosi, A.
dc.contributor.authorFonseca, M. V.
dc.contributor.authorColin, P.
dc.contributor.authorColombo, E.
dc.contributor.authorContreras, J. L.
dc.contributor.authorCortina, J.
dc.contributor.authorCossio, L.
dc.contributor.authorCovino, S.
dc.contributor.authorDazzi, F.
dc.contributor.authorPeruzzo, L.
dc.contributor.authorDe Angelis, A.
dc.contributor.authorDe Caneva, G.
dc.contributor.authorDe Cea del Pozo, E.
dc.contributor.authorFont, L.
dc.contributor.authorDelgado Mendez, C.
dc.contributor.authorDe Lotto, B.
dc.contributor.authorDiago Ortega, A.
dc.contributor.authorDoert, M.
dc.contributor.authorDomínguez, A.
dc.contributor.authorDominis Prester, D.
dc.contributor.authorLópez, M.
dc.contributor.authorDorner, D.
dc.contributor.authorDoro, M.
dc.contributor.authorFruck, C.
dc.contributor.authorGarcía López, R. J.
dc.contributor.authorGarczarczyk, M.
dc.contributor.authorGarrido, D.
dc.contributor.authorGiavitto, G.
dc.contributor.authorPerez-Torres, M. A.
dc.contributor.authorGodinovic, N.
dc.contributor.authorHadasch, D.
dc.contributor.authorLópez-Oramas, A.
dc.contributor.authorHäfner, D.
dc.contributor.authorHerrero, A.
dc.contributor.authorHildebrand, D.
dc.contributor.authorHirotani, K.
dc.contributor.authorHöhne-Mönch, D.
dc.contributor.authorHose, J.
dc.contributor.authorHrupec, D.
dc.contributor.authorJogler, T.
dc.contributor.authorPersic, M.
dc.contributor.authorKellermann, H.
dc.contributor.authorLorenz, E.
dc.contributor.authorKlepser, S.
dc.contributor.authorKrähenbühl, T.
dc.contributor.authorKrause, J.
dc.contributor.authorKushida, J.
dc.contributor.authorLa Barbera, A.
dc.contributor.authorLelas, D.
dc.contributor.authorLeonardo, E.
dc.contributor.authorLindfors, E.
dc.contributor.authorMakariev, M.
dc.contributor.authorManeva, G.
dc.contributor.authorMankuzhiyil, N.
dc.contributor.authorMannheim, K.
dc.contributor.authorMaraschi, L.
dc.contributor.authorSitarek, J.
dc.contributor.authorMarcote, B.
dc.contributor.authorMariotti, M.
dc.contributor.authorPilia, M.
dc.contributor.authorMartínez, M.
dc.contributor.authorMazin, D.
dc.contributor.authorMeucci, M.
dc.contributor.authorMiranda, J. M.
dc.contributor.authorMirzoyan, R.
dc.contributor.authorMoldón, J.
dc.contributor.authorMoralejo, A.
dc.contributor.authorBiland, A.
dc.contributor.authorMunar-Adrover, P.
dc.contributor.authorNieto, D.
dc.contributor.authorNilsson, K.
dc.contributor.authorPochon, J.
dc.contributor.authorOrito, R.
dc.contributor.authorOtte, N.
dc.contributor.authorOya, I.
dc.contributor.authorPaneque, D.
dc.contributor.authorPaoletti, R.
dc.contributor.authorPardo, S.
dc.contributor.authorSnidaric, I.
dc.contributor.authorParedes, J. M.
dc.contributor.authorPartini, S.
dc.contributor.authorPrada, F.
dc.contributor.authorPrada Moroni, P. G.
dc.contributor.authorPrandini, E.
dc.contributor.authorPuerto Gimenez, I.
dc.contributor.authorPuljak, I.
dc.contributor.authorBerger, K.
dc.contributor.authorReichardt, I.
dc.contributor.authorReinthal, R.
dc.contributor.authorSobczynska, D.
dc.contributor.authorRhode, W.
dc.contributor.authorRibó, M.
dc.contributor.authorRico, J.
dc.contributor.authorRissi, M.
dc.contributor.authorRügamer, S.
dc.contributor.authorSaggion, A.
dc.contributor.authorSaito, K.
dc.contributor.authorSaito, T. Y.
dc.contributor.authorBernardini, E.
dc.contributor.authorSalvati, M.
dc.contributor.authorSpanier, F.
dc.contributor.authorSatalecka, K.
dc.contributor.authorScalzotto, V.
dc.contributor.authorScapin, V.
dc.contributor.authorSchultz, C.
dc.contributor.authorSchweizer, T.
dc.contributor.authorShayduk, M.
dc.contributor.authorShore, S. N.
dc.contributor.authorSillanpää, A.
dc.contributor.authorSpiro, S.
dc.contributor.authorStamatescu, V.
dc.contributor.authorStamerra, A.
dc.contributor.authorSteinke, B.
dc.contributor.authorStorz, J.
dc.contributor.authorEisenacher, D.
dc.contributor.authorStrah, N.
dc.contributor.authorSuric, T.
dc.contributor.authorBlanch, O.
dc.contributor.authorTakalo, L.
dc.contributor.authorTakami, H.
dc.contributor.authorTavecchio, F.
dc.contributor.authorTemnikov, P.
dc.contributor.authorTerzic, T.
dc.contributor.authorTescaro, D.
dc.contributor.authorTeshima, M.
dc.contributor.authorElsaesser, D.
dc.contributor.authorTibolla, O.
dc.contributor.authorTorres, D. F.
dc.contributor.authorTreves, A.
dc.contributor.authorBock, R. K.
dc.contributor.authorUellenbeck, M.
dc.contributor.authorVankov, H.
dc.contributor.authorVogler, P.
dc.contributor.authorWagner, R. M.
dc.contributor.authorWeitzel, Q.
dc.date.accessioned2012-03-05T15:38:38Z
dc.date.available2012-03-05T15:38:38Z
dc.date.issued2011-01-01
dc.description.abstractWe report on the observation of γ-rays above 25 GeV from the Crab pulsar (PSR B0532+21) using the MAGIC I telescope. Two data sets from observations during the winter period 2007/2008 and 2008/2009 are used. In order to discuss the spectral shape from 100 MeV to 100 GeV, one year of public Fermi Large Area Telescope (Fermi-LAT) data are also analyzed to complement the MAGIC data. The extrapolation of the exponential cutoff spectrum determined with the Fermi-LAT data is inconsistent with MAGIC measurements, which requires a modification of the standard pulsar emission models. In the energy region between 25 and 100 GeV, the emission in the P1 phase (from –0.06 to 0.04, location of the main pulse) and the P2 phase (from 0.32 to 0.43, location of the interpulse) can be described by power laws with spectral indices of –3.1 ± 1.0stat ± 0.3syst and –3.5 ± 0.5stat ± 0.3syst, respectively. Assuming an asymmetric Lorentzian for the pulse shape, the peak positions of the main pulse and the interpulse are estimated to be at phases –0.009 ± 0.007 and 0.393 ± 0.009, while the full widths at half-maximum are 0.025 ± 0.008 and 0.053 ± 0.015, respectively.en
dc.identifier.doi10.1088/0004-637X/742/1/43
dc.identifier.urihttp://hdl.handle.net/2003/29370
dc.identifier.urihttp://dx.doi.org/10.17877/DE290R-4316
dc.identifier.urlhttp://dx.doi.org/10.1088/0004-637X/742/1/43
dc.language.isoende
dc.publisherInstitute of Physicsen
dc.relation.ispartofseriesThe Astrophysical Journal ; Volume 727, Number 1en
dc.rights© IOP Publishing 2012
dc.subject.ddc004
dc.titleObservations of the Crab Pulsar between 25 and 100 GeV with the MAGIC I Telescopeen
dc.typeTextde
dc.type.publicationtypearticlede
dcterms.accessRightsopen access

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