F. AceroM. AckermannM. AjelloL. BaldiniJ. BalletG. BarbielliniD. BastieriR. BellazziniE. BissaldiR. D. BlandfordE. D. BloomR. BoninoE. BottaciniT. J. BrandtJ. BregeonP. BruelR. BuehlerS. BusonG. A. CaliandroR. A. CameronR. CaputoM. CaragiuloP. A. CaraveoJ. M. CasandjianE. CavazzutiC. CecchiA. ChekhtmanJ. ChiangG. ChiaroS. CipriniR. ClausJ. M. CohenJ. Cohen-TanugiL. R. CominskyB. CondonJ. ConradS. CutiniF. D'AmmandoA. De AngelisF. De PalmaR. DesianteS. W. DigelL. Di VenereP. S. DrellA. Drlica-WagnerC. FavuzziE. C. FerraraA. FranckowiakY. FukazawaS. FunkP. FuscoF. GarganoD. GasparriniN. GigliettoP. GiommiF. GiordanoM. GirolettiT. GlanzmanG. GodfreyG. A. Gomez-VargasI. A. GrenierM. H. GrondinL. GuillemotS. GuiriecM. GustafssonD. HadaschA. K. HardingM. HayashidaE. HaysJ. W. HewittA. B. HillD. HoranX. HouInstitut de Recherche sur les Lois Fondamentales de l'UniversDeutsche Elektronen-SynchrotronClemson UniversityUniversità di PisaKavli Institute for Particle Astrophysics and CosmologyIstituto Nazionale di Fisica Nucleare, RomaUniversita degli Studi di TriesteIstituto Nazionale Di Fisica Nucleare, Sezione di PadovaUniversità degli Studi di PadovaIstituto Nazionale Di Fisica Nucleare, Sezione di PisaUniversità degli Studi di TorinoNASA Goddard Space Flight CenterLaboratoire Univers et Particules de MontpellierLaboratoire Leprince-RinguetConsorzio Interuniversitario per la Fisica Spaziale (CIFS)Santa Cruz Institute for Particle PhysicsINAF Istituto di Astrofisica Spaziale e Fisica Cosmica, MilanAgenzia Spaziale ItalianaUniversita degli Studi di PerugiaGeorge Mason University, Fairfax CampusOsservatorio Astronomico di RomaUniversity of MarylandSonoma State UniversityCentre d'Etudes Nucleaires de Bordeaux GradignanStockholms universitetOskar Klein Centre for Cosmoparticle PhysicsKungl. VetenskapsakademienIstituto Di Radioastronomia, BolognaAlma Mater Studiorum Università di BolognaUniversita degli Studi di UdineUniversità degli Studi di Napoli Federico IIUniversità degli Studi di BariFermi National Accelerator LaboratoryHiroshima UniversityErlangen Centre for Astroparticle PhysicsPontificia Universidad Católica de ChileUniversite d'OrleansInstitut National des Sciences de l'UniversUniversität GöttingenMedizinische Universitat InnsbruckUniversity of TokyoUniversity of North FloridaUniversity of SouthamptonChinese Academy of SciencesOsservatorio Astronomico di TriesteUniversity Science Institute ReykjavikIbaraki UniversityWaseda UniversityAustralia Telescope National FacilityCNRS Centre National de la Recherche ScientifiqueUniversite de ToulouseTwitter, Inc.The Royal Institute of Technology (KTH)Universitat Autònoma de BarcelonaNaval Research Laboratory2018-12-112019-03-142018-12-112019-03-142016-05-01Astrophysical Journal, Supplement Series. Vol.224, No.1 (2016)006700492-s2.0-84977648287https://repository.li.mahidol.ac.th/handle/123456789/43566© 2016. The American Astronomical Society. All rights reserved. To uniformly determine the properties of supernova remnants (SNRs) at high energies, we have developed the first systematic survey at energies from 1 to 100 GeV using data from the Fermi Large Area Telescope (LAT). Based on the spatial overlap of sources detected at GeV energies with SNRs known from radio surveys, we classify 30 sources as likely GeV SNRs. We also report 14 marginal associations and 245 flux upper limits. A mock catalog in which the positions of known remnants are scrambled in Galactic longitude allows us to determine an upper limit of 22% on the number of GeV candidates falsely identified as SNRs. We have also developed a method to estimate spectral and spatial systematic errors arising from the diffuse interstellar emission model, a key component of all Galactic Fermi LAT analyses. By studying remnants uniformly in aggregate, we measure the GeV properties common to these objects and provide a crucial context for the detailed modeling of individual SNRs. Combining our GeV results with multiwavelength (MW) data, including radio, X-ray, and TeV, we demonstrate the need for improvements to previously sufficient, simple models describing the GeV and radio emission from these objects. We model the GeV and MW emission from SNRs in aggregate to constrain their maximal contribution to observed Galactic cosmic rays.Mahidol UniversityEarth and Planetary SciencesArticleSCOPUS10.3847/0067-0049/224/1/8