February
2016
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2016A&A...586A.134P
Authors
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Planck Collaboration
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Arnaud, M.
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Ashdown, M.
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Atrio-Barandela, F.
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Aumont, J.
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Baccigalupi, C.
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Banday, A. J.
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Barreiro, R. B.
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Battaner, E.
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Benabed, K.
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Benoit-Lévy, A.
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Bernard, J. -P.
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Bersanelli, M.
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Bielewicz, P.
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Bobin, J.
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Bond, J. R.
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Borrill, J.
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Bouchet, F. R.
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Brogan, C. L.
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Burigana, C.
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Cardoso, J. -F.
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Catalano, A.
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Chamballu, A.
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Chiang, H. C.
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Christensen, P. R.
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Colombi, S.
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Colombo, L. P. L.
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Crill, B. P.
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Curto, A.
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Cuttaia, F.
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Davies, R. D.
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Davis, R. J.
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de Bernardis, P.
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de Rosa, A.
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de Zotti, G.
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Delabrouille, J.
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Désert, F. -X.
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Dickinson, C.
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Diego, J. M.
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Donzelli, S.
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Doré, O.
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Dupac, X.
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Enßlin, T. A.
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Eriksen, H. K.
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Finelli, F.
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Forni, O.
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Frailis, M.
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Fraisse, A. A.
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Franceschi, E.
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Galeotta, S.
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Ganga, K.
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Giard, M.
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Giraud-Héraud, Y.
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González-Nuevo, J.
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Górski, K. M.
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Gregorio, A.
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Gruppuso, A.
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Hansen, F. K.
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Harrison, D. L.
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Hernández-Monteagudo, C.
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Herranz, D.
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Hildebrandt, S. R.
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Hobson, M.
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Holmes, W. A.
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Huffenberger, K. M.
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Jaffe, A. H.
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Jaffe, T. R.
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Keihänen, E.
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Keskitalo, R.
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Kisner, T. S.
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Kneissl, R.
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Knoche, J.
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Kunz, M.
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Kurki-Suonio, H.
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Lähteenmäki, A.
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Lamarre, J. -M.
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Lasenby, A.
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Lawrence, C. R.
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Leonardi, R.
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Liguori, M.
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Lilje, P. B.
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Linden-Vørnle, M.
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López-Caniego, M.
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Lubin, P. M.
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Maino, D.
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Maris, M.
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Marshall, D. J.
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Martin, P. G.
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Martínez-González, E.
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Masi, S.
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Matarrese, S.
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Mazzotta, P.
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Melchiorri, A.
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Mendes, L.
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Mennella, A.
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Migliaccio, M.
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Miville-Deschênes, M. -A.
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Moneti, A.
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Montier, L.
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Morgante, G.
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Mortlock, D.
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Munshi, D.
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Murphy, J. A.
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Naselsky, P.
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Nati, F.
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Noviello, F.
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Novikov, D.
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Novikov, I.
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Oppermann, N.
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Oxborrow, C. A.
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Pagano, L.
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Pajot, F.
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Paladini, R.
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Pasian, F.
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Peel, M.
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Perdereau, O.
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Perrotta, F.
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Piacentini, F.
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Piat, M.
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Pietrobon, D.
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Plaszczynski, S.
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Pointecouteau, E.
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Polenta, G.
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Popa, L.
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Pratt, G. W.
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Puget, J. -L.
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Rachen, J. P.
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Reach, W. T.
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Reich, W.
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Reinecke, M.
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Remazeilles, M.
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Renault, C.
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Rho, J.
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Ricciardi, S.
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Riller, T.
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Ristorcelli, I.
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Rocha, G.
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Rosset, C.
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Roudier, G.
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Rusholme, B.
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Sandri, M.
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Savini, G.
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Scott, D.
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Stolyarov, V.
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Sutton, D.
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Suur-Uski, A. -S.
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Sygnet, J. -F.
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Tauber, J. A.
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Terenzi, L.
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Toffolatti, L.
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Tomasi, M.
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Tristram, M.
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Tucci, M.
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Umana, G.
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Valenziano, L.
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Valiviita, J.
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Van Tent, B.
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Vielva, P.
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Villa, F.
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Wade, L. A.
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Yvon, D.
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Zacchei, A.
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Zonca, A.
Abstract
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The all-sky Planck survey in 9 frequency bands was used to search for emission from all 274 known Galactic supernova remnants. Of these, 16 were detected in at least two Planck frequencies. The radio-through-microwave spectral energy distributions were compiled to determine the mechanism for microwave emission. In only one case, IC 443, is there high-frequency emission clearly from dust associated with the supernova remnant. In all cases, the low-frequency emission is from synchrotron radiation. As predicted for a population of relativistic particles with energy distribution that extends continuously to high energies, a single power law is evident for many sources, including the Crab and PKS 1209-51/52. A decrease in flux density relative to the extrapolation of radio emission is evident in several sources. Their spectral energy distributions can be approximated as broken power laws, Sν ∝ ν-α, with the spectral index, α, increasing by 0.5-1 above a break frequency in the range 10-60 GHz. The break could be due to synchrotron losses.
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