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Authors: F. Acero
M. Ackermann
M. Ajello
L. Baldini
J. Ballet
G. Barbiellini
D. Bastieri
R. Bellazzini
E. Bissaldi
R. D. Blandford
E. D. Bloom
R. Bonino
E. Bottacini
T. J. Brandt
J. Bregeon
P. Bruel
R. Buehler
S. Buson
G. A. Caliandro
R. A. Cameron
R. Caputo
M. Caragiulo
P. A. Caraveo
J. M. Casandjian
E. Cavazzuti
C. Cecchi
A. Chekhtman
J. Chiang
G. Chiaro
S. Ciprini
R. Claus
J. M. Cohen
J. Cohen-Tanugi
L. R. Cominsky
B. Condon
J. Conrad
S. Cutini
F. D'Ammando
A. De Angelis
F. De Palma
R. Desiante
S. W. Digel
L. Di Venere
P. S. Drell
A. Drlica-Wagner
C. Favuzzi
E. C. Ferrara
A. Franckowiak
Y. Fukazawa
S. Funk
P. Fusco
F. Gargano
D. Gasparrini
N. Giglietto
P. Giommi
F. Giordano
M. Giroletti
T. Glanzman
G. Godfrey
G. A. Gomez-Vargas
I. A. Grenier
M. H. Grondin
L. Guillemot
S. Guiriec
M. Gustafsson
D. Hadasch
A. K. Harding
M. Hayashida
E. Hays
J. W. Hewitt
A. B. Hill
D. Horan
X. Hou
Institut de Recherche sur les Lois Fondamentales de l'Univers
Deutsche Elektronen-Synchrotron
Clemson University
Università di Pisa
Kavli Institute for Particle Astrophysics and Cosmology
Istituto Nazionale di Fisica Nucleare, Roma
Universita degli Studi di Trieste
Istituto Nazionale Di Fisica Nucleare, Sezione di Padova
Università degli Studi di Padova
Istituto Nazionale Di Fisica Nucleare, Sezione di Pisa
Università degli Studi di Torino
NASA Goddard Space Flight Center
Laboratoire Univers et Particules de Montpellier
Laboratoire Leprince-Ringuet
Consorzio Interuniversitario per la Fisica Spaziale (CIFS)
Santa Cruz Institute for Particle Physics
INAF Istituto di Astrofisica Spaziale e Fisica Cosmica, Milan
Agenzia Spaziale Italiana
Universita degli Studi di Perugia
George Mason University, Fairfax Campus
Osservatorio Astronomico di Roma
University of Maryland
Sonoma State University
Centre d'Etudes Nucleaires de Bordeaux Gradignan
Stockholms universitet
Oskar Klein Centre for Cosmoparticle Physics
Kungl. Vetenskapsakademien
Istituto Di Radioastronomia, Bologna
Alma Mater Studiorum Università di Bologna
Universita degli Studi di Udine
Università degli Studi di Napoli Federico II
Università degli Studi di Bari
Fermi National Accelerator Laboratory
Hiroshima University
Erlangen Centre for Astroparticle Physics
Pontificia Universidad Católica de Chile
Universite d'Orleans
Institut National des Sciences de l'Univers
Universität Göttingen
Medizinische Universitat Innsbruck
University of Tokyo
University of North Florida
University of Southampton
Chinese Academy of Sciences
Osservatorio Astronomico di Trieste
University Science Institute Reykjavik
Ibaraki University
Waseda University
Australia Telescope National Facility
CNRS Centre National de la Recherche Scientifique
Universite de Toulouse
Twitter, Inc.
The Royal Institute of Technology (KTH)
Universitat Autònoma de Barcelona
Naval Research Laboratory
Keywords: Earth and Planetary Sciences
Issue Date: 1-May-2016
Citation: Astrophysical Journal, Supplement Series. Vol.224, No.1 (2016)
Abstract: © 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.
ISSN: 00670049
Appears in Collections:Scopus 2016-2017

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