September
2013
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2013A&A...557A..53P
Authors
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Planck Collaboration
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Ade, P. A. R.
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Aghanim, N.
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Alves, M. I. R.
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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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Balbi, A.
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Banday, A. J.
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Barreiro, R. B.
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Bartlett, J. G.
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Battaner, E.
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Bedini, L.
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Benabed, K.
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Benoît, A.
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Bernard, J. -P.
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Bersanelli, M.
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Bonaldi, A.
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Bond, J. R.
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Borrill, J.
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Bouchet, F. R.
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Boulanger, F.
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Burigana, C.
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Butler, R. C.
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Cabella, P.
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Cardoso, J. -F.
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Chen, X.
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Chiang, L. -Y.
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Christensen, P. R.
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Clements, D. L.
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Colombi, S.
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Colombo, L. P. L.
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Coulais, 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 Gasperis, G.
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de Zotti, G.
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Delabrouille, J.
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Dickinson, C.
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Diego, J. M.
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Dobler, G.
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Dole, H.
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Donzelli, S.
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Doré, O.
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Douspis, M.
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Dupac, X.
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Enßlin, T. A.
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Finelli, F.
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Forni, O.
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Frailis, M.
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Franceschi, E.
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Galeotta, S.
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Ganga, K.
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Génova-Santos, R. T.
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Ghosh, T.
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Giard, M.
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Giardino, G.
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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.
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Hernández-Monteagudo, C.
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Hildebrandt, S. R.
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Hivon, E.
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Hobson, M.
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Holmes, W. A.
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Hornstrup, A.
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Hovest, W.
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Huffenberger, K. M.
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Jaffe, T. R.
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Jaffe, A. H.
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Juvela, M.
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Keihänen, E.
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Keskitalo, R.
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Kisner, T. S.
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Knoche, J.
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Kunz, M.
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Kurki-Suonio, H.
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Lagache, G.
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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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Leach, S.
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Leonardi, R.
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Lilje, P. B.
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Linden-Vørnle, M.
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Lubin, P. M.
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Macías-Pérez, J. F.
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Maffei, B.
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Maino, D.
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Mandolesi, N.
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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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Massardi, M.
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Matarrese, S.
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Mazzotta, P.
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Melchiorri, A.
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Mennella, A.
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Mitra, S.
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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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Natoli, P.
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Nørgaard-Nielsen, H. U.
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Noviello, F.
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Novikov, D.
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Novikov, I.
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Osborne, S.
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Oxborrow, C. A.
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Pajot, F.
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Paladini, R.
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Paoletti, D.
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Peel, M.
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Perotto, L.
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Perrotta, F.
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Piacentini, F.
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Piat, M.
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Pierpaoli, E.
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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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Poutanen, T.
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Pratt, G. W.
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Prunet, S.
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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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Rebolo, R.
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Reinecke, M.
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Renault, C.
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Ricciardi, S.
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Ristorcelli, I.
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Rocha, G.
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Rosset, C.
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Rubiño-Martín, J. A.
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Rusholme, B.
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Salerno, E.
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Sandri, M.
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Savini, G.
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Scott, D.
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Spencer, L.
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Stolyarov, V.
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Sudiwala, R.
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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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Tibbs, C. T.
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Toffolatti, L.
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Tomasi, M.
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Tristram, M.
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Valenziano, L.
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Van Tent, B.
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Varis, J.
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Vielva, P.
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Villa, F.
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Vittorio, N.
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Wade, L. A.
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Wandelt, B. D.
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Ysard, N.
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Yvon, D.
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Zacchei, A.
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Zonca, A.
Abstract
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We perform an analysis of the diffuse low-frequency Galactic components in the southern part of the Gould Belt system (130° ≤ l ≤ 230° and -50° ≤ b ≤ -10°). Strong ultra-violet flux coming from the Gould Belt super-association is responsible for bright diffuse foregrounds that we observe from our position inside the system and that can help us improve our knowledge of the Galactic emission. Free-free emission and anomalous microwave emission (AME) are the dominant components at low frequencies (ν < 40 GHz), while synchrotron emission is very smooth and faint. We separated diffuse free-free emission and AME from synchrotron emission and thermal dust emission by using Planck data, complemented by ancillary data, using the correlated component analysis (CCA) component-separation method and we compared our results with the results of cross-correlation of foreground templates with the frequency maps. We estimated the electron temperature Te from Hα and free-free emission using two methods (temperature-temperature plot and cross-correlation) and obtained Te ranging from 3100 to 5200K for an effective fraction of absorbing dust along the line of sight of 30% (fd = 0.3). We estimated the frequency spectrum of the diffuse AME and recovered a peak frequency (in flux density units) of 25.5 ± 1.5 GHz. We verified the reliability of this result with realistic simulations that include biases in the spectral model for the AME and in the free-free template. By combining physical models for vibrational and rotational dust emission and adding the constraints from the thermal dust spectrum from Planck and IRAS, we are able to present a good description of the AME frequency spectrum for plausible values of the local density and radiation field.
Appendices are available in electronic form at
http://www.aanda.org
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