J/ApJ/799/86ivo://CDS.VizieR/J/ApJ/799/86doi:10.26093/cds/vizier.17990086CDSAckermann M.Ajello M.Albert A.Atwood W.B.Baldini L.Ballet J.,Barbiellini G.Bastieri D.Bechtol K.Bellazzini R.Bissaldi E.,Blandford R.D.Bloom E.D.Bottacini E.Brandt T.J.Bregeon J.,Bruel P.Buehler R.Buson S.Caliandro G.A.Cameron R.A.Caragiulo M.,Caraveo P.A.Cavazzuti E.Cecchi C.Charles E.Chekhtman A.Chiang J.,Chiaro G.Ciprini S.Claus R.Cohen-Tanugi J.Conrad J.Cuoco A.,Cutini S.D'Ammando F.de Angelis A.de Palma F.Dermer C.D.,Digel S.W.do Couto e Silva E.Drell P.S.Favuzzi C.Ferrara E.C.,Focke W.B.Franckowiak A.Fukazawa Y.Funk S.Fusco P.Gargano F.,Gasparrini D.Germani S.Giglietto N.Giommi P.Giordano F.,Giroletti M.Godfrey G.Gomez-Vargas G.A.Grenier I.A.Guiriec S.,Gustafsson M.Hadasch D.Hayashi K.Hays E.Hewitt J.W.Ippoliti P.,Jogler T.Johannesson G.Johnson A.S.Johnson W.N.Kamae T.,Kataoka J.Knodlseder J.Kuss M.Larsson S.Latronico L.Li J.Li L.,Longo F.Loparco F.Lott B.Lovellette M.N.Lubrano P.Madejski G.M.,Manfreda A.Massaro F.Mayer M.Mazziotta M.N.McEnery J.E.,Michelson P.F.Mitthumsiri W.Mizuno T.Moiseev A.A.Monzani M.E.,Morselli A.Moskalenko I.V.Murgia S.Nemmen R.Nuss E.Ohsugi T.,Omodei N.Orlando E.Ormes J.F.Paneque D.Panetta J.H.Perkins J.S.,Pesce-Rollins M.Piron F.Pivato G.Porter T.A.Raino S.Rando R.,Razzano M.Razzaque S.Reimer A.Reimer O.Reposeur T.Ritz S.,Romani R.W.Sanchez-Conde M.Schaal M.Schulz A.Sgro C.Siskind E.J.,Spandre G.Spinelli P.Strong A.W.Suson D.J.Takahashi H.,Thayer J.G.Thayer J.B.Tibaldo L.Tinivella M.Torres D.F.Tosti G.,Troja E.Uchiyama Y.Vianello G.Werner M.Winer B.L.Wood K.S.,Wood M.Zaharijas G.Zimmer S.2015-07-29T18:03:48Z2015-07-06T09:49:41ZCDS support team

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

cds-question@unistra.frgamma-ray-astronomyThe {gamma}-ray sky can be decomposed into individually detected sources, diffuse emission attributed to the interactions of Galactic cosmic rays with gas and radiation fields, and a residual all-sky emission component commonly called the isotropic diffuse {gamma}-ray background (IGRB). The IGRB comprises all extragalactic emissions too faint or too diffuse to be resolved in a given survey, as well as any residual Galactic foregrounds that are approximately isotropic. The first IGRB measurement with the Large Area Telescope (LAT) on board the Fermi Gamma-ray Space Telescope (Fermi) used 10 months of sky-survey data and considered an energy range between 200MeV and 100GeV. Improvements in event selection and characterization of cosmic-ray backgrounds, better understanding of the diffuse Galactic emission (DGE), and a longer data accumulation of 50 months allow for a refinement and extension of the IGRB measurement with the LAT, now covering the energy range from 100MeV to 820GeV. The IGRB spectrum shows a significant high-energy cutoff feature and can be well described over nearly four decades in energy by a power law with exponential cutoff having a spectral index of 2.32+/-0.02 and a break energy of (279+/-52)GeV using our baseline DGE model. The total intensity attributed to the IGRB is (7.2+/-0.6)x10^-6^/cm2/s/sr above 100MeV, with an additional +15%/-30% systematic uncertainty due to the Galactic diffuse foregrounds.2015ApJ...799...86Ahttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/ApJ/799/86CatalogResearchIsServedByTAP VizieR generic servicerelated-toVIII/76 : Leiden/Argentine/Bonn (LAB) Survey of Galactic HI (Kalberla+ 2005)J/ApJS/209/34 : The first Fermi-LAT >10GeV catalog (1FHL) (Ackermann+, 2013)J/ApJS/208/17 : 2nd Fermi LAT cat. of gamma-ray pulsars (2PC) (Abdo+, 2013)J/ApJS/199/31 : Fermi LAT second source catalog (2FGL) (Nolan+, 2012)J/ApJ/743/171 : The 2LAC catalog (Ackermann+, 2011)J/A+A/534/A54 : GALPROP programme (Strong+, 2011)J/ApJS/171/61 : All-Sky Survey of Flat-Spectrum Radio Sources (Healey+, 2007)J/MNRAS/372/777 : Parkes Multibeam Pulsar Survey. VI. (Lorimer+, 2006)http://fermi.gsfc.nasa.gov/ssc/ : Fermi Science Support Center home pagehttp://www.hawc-observatory.org/ : High-Altitude Water Cherenkov Observatoryhttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/ApJ/799/86https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/ApJ/799/86http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/ApJ/799/86https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/ApJ/799/86https://vizier.iucaa.in/viz-bin/votable?-source=J/ApJ/799/86http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/ApJ/799/86GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapGamma-raydefaultJ/ApJ/799/86/table3Isotropic diffuse {gamma}-ray background (IGRB) and total extragalactic {gamma}-ray background (EGB) intensitiesModel[A-C] Model (1)meta.notecharrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintEmin[100/579262] Lower energy range of bandMeVinstr.bandwidth;stat.mindoubleEmax[141/819200] Upper energy range of bandMeVinstr.bandwidth;stat.maxdoublefIGRBIntegrated IGRB flux in bandph.cm**-2.s**-1.sr**-1phot.flux.density;em.gamma.harddoubleE_fIGRBUpper uncertainty in fIGRB (2)ph.cm**-2.s**-1.sr**-1stat.error;stat.maxdoublee_fIGRBLower uncertainty in fIGRB (2)ph.cm**-2.s**-1.sr**-1stat.errordoubleEfIGRBUpper uncertainty in fIGRB from foreground modelingph.cm**-2.s**-1.sr**-1stat.errordoubleefIGRBLower uncertainty in fIGRB from foreground modelingph.cm**-2.s**-1.sr**-1stat.errordoublefEGBIntegrated total EGB in band (3)ph.cm**-2.s**-1.sr**-1phot.flux.density;em.gamma.harddoubleE_fEGBUpper uncertainty in fEGB (2)ph.cm**-2.s**-1.sr**-1stat.error;stat.maxdoublee_fEGBLower uncertainty in fEGB (2)ph.cm**-2.s**-1.sr**-1stat.errordoubleEfEGBUpper uncertainty in fEGB from foreground modelingph.cm**-2.s**-1.sr**-1stat.errordoubleefEGBLower uncertainty in fEGB from foreground modelingph.cm**-2.s**-1.sr**-1stat.errordoublefsrcIntegrated flux of sources in band (4)ph.cm**-2.s**-1.sr**-1phot.flux.density;em.gamma.harddoubleE_fsrcUpper uncertainty in fsrcph.cm**-2.s**-1.sr**-1stat.error;stat.maxdoublee_fsrcLower uncertainty in fsrcph.cm**-2.s**-1.sr**-1stat.errordouble