J/A+A/549/A23ivo://CDS.VizieR/J/A+A/549/A23doi:10.26093/cds/vizier.35490023CDSAleksic J.Antonelli L.A.Antoranz P.Asensio M.Barres de Almeida U.,Barrio J.A.Becerra Gonzalez J.Bednarek W.Berger K.Bernardini E.,Biland A.Blanch O.Bock R.K.Boller A.Bonnoli G.Borla Tridon D.,Bretz T.Carmona E.Carosi A.Colin P.Colombo E.Contreras J.L.,Cortina J.Cossio L.Covino S.Da Vela P.Dazzi F.De Angelis A.,De Caneva G.De Cea del Pozo E.De Lotto B.Delgado Mendez C.,Diago Ortega A.Doert M.Dominis Prester D.Dorner D.Doro M.,Eisenacher D.Elsaesser D.Ferenc D.Fonseca M.V.Font L.Fruck C.,Garcia Lopez R.J.Garczarczyk M.Garrido Terrats D.Gaug M.Giavitto G.,Godinovic N.Gonzalez Munoz A.Gozzini S.R.Hadamek A.Hadasch D.,Hafner D.Herrero A.Hose J.Hrupec D.Huber B.Jankowski F.,Jogler T.Kadenius V.Klepser S.Knoetig M.L.Krahenbuhl T.Krause J.,Kushida J.La Barbera A.Lelas D.Leonardo E.Lewandowska N.,Lindfors E.Lombardi S.Lopez M.Lopez-Coto R.Lopez-Oramas A.,Lorenz E.Makariev M.Maneva G.Mankuzhiyil N.Mannheim K.Maraschi L.,Marcote B.Mariotti M.Martinez M.Mazin D.Meucci M.Miranda J.M.,Mirzoyan R.Moldon J.Moralejo A.Munar-Adrover P.Niedzwiecki A.,Nieto D.Nilsson K.Nowak N.Orito R.Paiano S.Palatiello M.,Paneque D.Paoletti R.Paredes J.M.Partini S.Persic M.Pilia M.,Pochon J.Prada F.Prada Moroni P.G.Prandini E.Puljak I.,Reichardt I.Reinthal R.Rhode W.Ribo M.Rico J.Rugamer S.Saito K.,Saito T.Y.Salvati M.Satalecka K.Scalzotto V.Scapin V.Schultz C.,Saggion A.Schweizer T.Shore S.N.Sillanpaa A.Sitarek J.Snidaric I.,Sobczynska D.Spanier F.Spiro S.Stamatescu V.Stamerra A.Steinke B.,Storz J.Sun S.Suric T.Takalo L.Takami H.Tavecchio F.Temnikov P.,Terzic T.Tescaro D.Teshima M.Tibolla O.Torres D.F.Toyama T.,Treves A.Uellenbeck M.Vogler P.Wagner R.M.Weitzel Q.Zabalza V.,Zandanel F.Zanin R.Rea N.2017-05-12T14:14:42Z2012-12-10T09:11:24ZCDS support team

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

cds-question@unistra.frgamma-ray-astronomypulsarsMagnetars are an extreme, highly magnetized class of isolated neutron stars whose large X-ray luminosity is believed to be driven by their high magnetic field. Study for the first time the possible very high energy {gamma}-ray emission above 100GeV from magnetars, observing the sources 4U 0142+61 and 1E 2259+586.2013A&A...549A..23Ahttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/549/A23CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/549/A23https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/549/A23http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/549/A23https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/549/A23https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/549/A23http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/549/A23GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/A+A/549/A23/list (Information on map)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/549/A23/list?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/549/A23/list?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/549/A23/list?GETtext/xml+votable180.050000true345.2896558.900170.005555555555555556Associated datahttps://cdsarc.cds.unistra.fr/assocdata/?obs_collection=J/A+A/549/A236/14305https://cdsarc.cds.unistra.fr/viz-bin/moc/J/A+A/549/A23?format=asciiGamma-rayRadiodefaultJ/A+A/549/A23/listInformation on maprecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintRAJ2000Right Ascension of center (J2000)degpos.eq.ra;meta.mainDEJ2000Declination of center (J2000)degpos.eq.dec;meta.mainScaleScale of the image (38"/pix)arcsec/pixinstr.scalefloatNx[264] Number of pixels along X-axispixmeta.numberintNy[189] Number of pixels along Y-axispixmeta.numberintDownloadDownload the FITS filemeta.ref.urlcharFileNameName of FITS filemeta.id;meta.fitscharAssocDataAssociated Data web pagemeta.bib.pagecharJ/A+A/549/A23/fluxesHigh-energy flux limitsrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintE[200/20000] EnergyGeVintF1Flux of 4U 0142+61 at Eph.cm**-2.s**-1doubleF2Flux of 1E 2259+586 at Eph.cm**-2.s**-1double