J/A+A/565/L12ivo://CDS.VizieR/J/A+A/565/L12doi:10.26093/cds/vizier.35659012CDSAleksic J.Saito T.Y.Zanin R.Bonnefoy S.Hirotani K.,Ansoldi S.Antonelli L.A.Antoranz P.Babic A.Bangale P.,Barres de Almeida U.Barrio J.A.Becerra Gonzalez J.Bednarek W.,Bernardini E.Biasuzzi B.Biland A.Blanch O.Bonnoli G.Borracci F.,Bretz T.Carmona E.Carosi A.Colin P.Colombo E.Contreras J.L.,Cortina J.Covino S.Da Vela P.Dazzi F.De Angelis A.De Caneva G.,De Lotto B.Delgado Mendez C.Doert M.Dominis Prester D.Dorner D.,Doro M.Einecke S.Eisenacher D.Elsaesser D.Farina E.Ferenc D.,Fidalgo D.Fonseca M.V.Font L.Frantzen K.Fruck C.Garcia Lopez R.J.,Garczarczyk M.Garrido Terrats D.Gaug M.Godinovic N.,Gonzalez Munoz A.Gozzini S.R.Hadasch D.Hayashida M.Herrera J.,Herrero A.Hildebrand D.Hose J.Hrupec D.Idec W.Kadenius V.,Kellermann H.Kodani K.Konno Y.Krause J.Kubo H.Kushida J.,La Barbera A.Lelas D.Lewandowska N.Lindfors E.Lombardi S.Lopez M.,Lopez-Coto R.Lopez-Oramas A.Lorenz E.Lozano I.Makariev M.,Mallot K.Maneva G.Mankuzhiyil N.Mannheim K.Maraschi L.Marcote B.,Mariotti M.Martinez M.Mazin D.Menzel U.Miranda J.M.Mirzoyan R.,Moralejo A.Munar-Adrover P.Nakajima D.Niedzwiecki A.Nilsson K.,Nishijima K.Noda K.Nowak N.Orito R.Overkemping A.Paiano S.,Palatiello M.Paneque D.Paoletti R.Paredes J.M.Paredes-Fortuny X.,Partini S.Persic M.Prada Moroni P.G.Prandini E.Preziuso S.,Puljak I.Reinthal R.Rhode W.Ribo M.Rico J.Rodriguez Garcia J.,Rugamer S.Saggion A.Saito K.Satalecka K.Scalzotto V.Scapin V.,Schultz C.Schweizer T.Shore S.N.Sillanpaa A.Sitarek J.Snidaric I.,Sobczynska D.Spanier F.Stamatescu V.Stamerra A.Steinbring T.,Storz J.Strzys M.Sun S.Suric T.Takalo L.Takami H.Tavecchio F.,Temnikov P.Terzic T.Tescaro D.Teshima M.Thaele J.Tibolla O.,Torres D.F.Toyama T.Treves A.Uellenbeck M.Vogler P.Wagner R.M.2017-06-19T07:57:30Z2014-06-03T15:57:23ZCDS support team

CDS, Observatoire de Strasbourg, 11 rue de l'Universite, F-67000 Strasbourg, France

cds-question@unistra.frgamma-ray-astronomypulsarsThe Crab pulsar is the only astronomical pulsed source detected at very high energy (VHE, E>100GeV) gamma rays. The emission mechanism of VHE pulsation is not yet fully understood, although several theoretical models have been proposed. 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. We analyzed 135h 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 analyzed2014A&A...565L..12Ahttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/565/L12CatalogResearchIsServedByTAP VizieR generic servicerelated-toJ/A+AS/124/123 : Atlas of the Crab pulsar pulse profiles (Massaro+ 1997)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/565/L12https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/565/L12http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/565/L12https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/565/L12https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/565/L12http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/565/L12GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapGamma-rayRadiodefaultJ/A+A/565/L12/lcLight curves at 50-100GeV, 100-400GeV and 50-400GeVrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintNo[0/9] Line numbermeta.idintphi0[-1/1] Lower edge of phase bin (1)time.phasefloatphi1[-1/1] Upper edge of phase bin (1)time.phasefloatF50-100Flux amplitude at 50-100GeVctphot.count;em.gamma.hardfloate_F50-100Error of Flux amplitude at 50-100GeVctstat.errorfloatF100-400Flux amplitude at 100-400GeVctphot.count;em.gamma.hardfloate_F100-400Error of Flux amplitude at 100-400GeVctstat.errorfloatF50-400Flux amplitude at 50-400GeVctphot.count;em.gamma.hardfloate_F50-400Error of Flux amplitude at 50-400GeVctstat.errorfloat