December
2011
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2011A&A...536A..12P
Authors
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Planck Collaboration
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Aghanim, N.
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Arnaud, M.
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Ashdown, M.
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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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Bartelmann, M.
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Bartlett, J. G.
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Battaner, E.
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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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Bhatia, R.
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Bock, J. J.
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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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Brown, M. L.
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Bucher, M.
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Burigana, C.
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Cabella, P.
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Cardoso, J. -F.
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Catalano, A.
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Cayón, L.
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Challinor, A.
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Chamballu, A.
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Chiang, L. -Y.
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Chiang, C.
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Chon, G.
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Christensen, P. R.
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Churazov, E.
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Clements, D. L.
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Colafrancesco, S.
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Colombi, S.
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Couchot, F.
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Coulais, A.
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Crill, B. P.
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Cuttaia, F.
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da Silva, A.
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Dahle, H.
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Danese, L.
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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 Rosa, A.
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de Zotti, G.
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Delabrouille, J.
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Delouis, J. -M.
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Désert, F. -X.
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Diego, J. M.
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Dolag, K.
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Donzelli, S.
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Doré, O.
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Dörl, U.
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Douspis, M.
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Dupac, X.
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Efstathiou, G.
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Enßlin, T. A.
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Finelli, F.
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Flores-Cacho, I.
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Forni, O.
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Frailis, M.
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Franceschi, E.
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Fromenteau, S.
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Galeotta, S.
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Ganga, K.
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Génova-Santos, R. 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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Gratton, S.
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Gregorio, A.
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Gruppuso, A.
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Harrison, D.
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Henrot-Versillé, S.
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Hernández-Monteagudo, C.
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Herranz, D.
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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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Hovest, W.
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Hoyland, R. J.
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Huffenberger, K. M.
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Jaffe, A. H.
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Jones, W. C.
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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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Kneissl, R.
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Knox, L.
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Kurki-Suonio, H.
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Lagache, G.
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Lamarre, J. -M.
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Lasenby, A.
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Laureijs, R. J.
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Lawrence, C. R.
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Leach, S.
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Leonardi, R.
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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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Macías-Pérez, J. F.
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MacTavish, C. J.
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Maffei, B.
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Maino, D.
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Mandolesi, N.
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Mann, R.
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Maris, M.
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Marleau, F.
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Martínez-González, E.
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Masi, S.
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Matarrese, S.
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Matthai, F.
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Mazzotta, P.
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Mei, S.
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Melchiorri, A.
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Melin, J. -B.
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Mendes, L.
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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, A.
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Naselsky, P.
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Natoli, P.
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Netterfield, C. B.
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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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O'Dwyer, I. J.
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Osborne, S.
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Pajot, F.
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Pasian, F.
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Patanchon, G.
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Perdereau, O.
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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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Piffaretti, R.
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Plaszczynski, S.
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Pointecouteau, E.
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Polenta, G.
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Ponthieu, N.
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Poutanen, T.
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Pratt, G. W.
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Prézeau, G.
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Prunet, S.
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Puget, J. -L.
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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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Riller, T.
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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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Sandri, M.
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Savini, G.
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Schaefer, B. M.
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Scott, D.
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Seiffert, M. D.
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Shellard, P.
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Smoot, G. F.
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Starck, J. -L.
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Stivoli, F.
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Stolyarov, V.
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Sudiwala, R.
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Sunyaev, R.
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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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Torre, J. -P.
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Tristram, M.
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Tuovinen, J.
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Valenziano, L.
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Vibert, L.
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Vielva, P.
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Villa, F.
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Vittorio, N.
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Wandelt, B. D.
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White, S. D. M.
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White, M.
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Yvon, D.
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Zacchei, A.
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Zonca, A.
Abstract
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We present the Sunyaev-Zeldovich (SZ) signal-to-richness scaling relation (Y500 - N200) for the MaxBCG cluster catalogue. Employing a multi-frequency matched filter on the Planck sky maps, we measure the SZ signal for each cluster by adapting the filter according to weak-lensing calibrated mass-richness relations (N200 - M500). We bin our individual measurements and detect the SZ signal down to the lowest richness systems (N200 = 10) with high significance, achieving a detection of the SZ signal in systems with mass as low as M500 ≈ 5 × 1013 M⊙. The observed Y500 - N200 relation is well modeled by a power law over the full richness range. It has a lower normalisation at given N200 than predicted based on X-ray models and published mass-richness relations. An X-ray subsample, however, does conform to the predicted scaling, and model predictions do reproduce the relation between our measured bin-average SZ signal and measured bin-average X-ray luminosities. At fixed richness, we find an intrinsic dispersion in the Y500 - N200 relation of 60% rising to of order 100% at low richness. Thanks to its all-sky coverage, Planck provides observations for more than 13000 MaxBCG clusters and an unprecedented SZ/optical data set, extending the list of known cluster scaling laws to include SZ-optical properties. The data set offers essential clues for models of galaxy formation. Moreover, the lower normalisation of the SZ-mass relation implied by the observed SZ-richness scaling has important consequences for cluster physics and cosmological studies with SZ clusters.
Corresponding author: J. G. Bartlett, e-mail: bartlett@apc.univ-paris7.fr
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