*. +#, /01-234,-)5(678)1&9 4:)

*. +#, /01-234

. Auchettl, Les types de SNRs sont différenciés par les couleurs indiquées dans la légende. différents types de SNRs (à coquille, composites ou incertains) ainsi que pour les SNRs ?5 ? ? b ? 5 ? ) est bien avancé et les résultats obtenus avec les chaînes d'analyse allemande et française sont compatibles. Ces résultats peuvent être mis en regard des estimations de Cristofari et al. (2013), dont les travaux sont fondés sur l'hypothèse que les SNRs sont effectivement les sources des CRs galactiques. En partant de cette hypothèse, une efficacité d'accélération moyenne de ?10% par SNR a été estimée à partir d'une luminosité des CRs galactiques L M W ? 10 41 erg/s et en supposant un taux de trois supernovae par siècle dans la Galaxie. A partir d'un modèle phénoménologique d'accélération de particules, les SNRs ont été simulés par Monte Carlo, et le flux ? associé aux interactions p-p et Compton inverse (sur le CMB) a été estimé à partir de modèles de distribution de gaz CO et HI dans la Galaxie (se reporter à Cristofari et al. 2013, et aux références associées pour plus de détails) La sensibilité (quasiment uniforme), Figure 10.9 ? Distributions des significativités (à gauche) et des limites supérieures (à droite) H.E.S.S. pour les SNRs de l'échantillon sûr (en haut) et pour la totalité des SNRs situé dans le HGPS Katagiri Pivato Castro Katsuta Hewitt Gelfand Castro Castro et al. (2013b) 10.4 Conclusion Le travail d'analyse H.E.S.S. des SNRs situés dans les régions internes du plan galactique (?113 ? ? ? ? 75 ? nébuleuse du Crabe (Aharonian et al. 2005) a alors été utilisée pour estimer le nombre de SNRs détectables par H.E.S.S. au delà de 1 TeV. Cette procédure a été répétée pour plusieurs valeurs d'indices spectraux (p=2.1-2.4) des distributions des particules accélérées au choc des SNRs et pour deux valeurs du rapport électron-sur-proton, 2010.

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