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Aleksic, J; Alvarez, E A; Antonelli, L A; Antoranz, P; Asensio, M; Backes, M; deAlmeida, U Barres; Barrio, J A; Bastieri, D; Gonzalez, J Becerra; Paneque, D; Paoletti, R; Pardo, S; Paredes, J M; Partini, S; Perez-Torres, M A; Persic, M; Pilia, M; Pochon, J; Prada, F; Bednarek, W; Moroni, P G Prada; Prandini, E; Gimenez, I Puerto; Puljak, I; Reichardt, I; Reinthal, R; Rhode, W; Ribo, M; Rico, J; Ruegamer, S; Berger, K; Saggion, A; Saito, K; Saito, T Y; Salvati, M; Satalecka, K; Scalzotto, V; Scapin, V; Schultz, C; Schweizer, T; Shore, S N; Bernardini, E; Sillanpaeae, A; Sitarek, J; Snidaric, I; Sobczynska, D; Spanier, F; Spiro, S; Stamatescu, V; et. al
Astronomy and astrophysics (Berlin), 05/2012, Letnik: 541Journal Article
The W51 complex hosts the supernova remnant W51C which is known to interact with the molecular clouds in the star forming region W51B. In addition, a possible pulsar wind nebula CXO J192318.5+140305 was found likely associated with the supernova remnant. Gamma-ray emission from this region was discovered by Fermi/LAT (between 0.2 and 50 GeV) and H.E.S.S. (>1 TeV). The aim is to determine the morphology of the very-high-energy gamma-ray emission of W51 and measure its spectral properties. The researches detect an extended emission of very-high-energy gamma rays, with a significance of 11 standard deviations. They extend the spectrum from the highest Fermi/LAT energies to ...5 TeV and find that it follows a single power law with an index of 2.58 ... 0.07stat ... 0.22syst. The main part of the emission coincides with the shocked cloud region, while we find a feature extending towards the pulsar wind nebula. (ProQuest: ... denotes formulae/symbols omitted.)
