November
2014
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2014A&A...571A..20P
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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Armitage-Caplan, C.
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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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Barrena, R.
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Bartlett, J. G.
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Battaner, E.
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Battye, R.
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Benabed, K.
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Benoît, A.
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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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Bikmaev, I.
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Blanchard, A.
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Bobin, J.
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Bock, J. J.
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Böhringer, H.
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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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Bourdin, H.
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Bridges, M.
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Brown, M. L.
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Bucher, M.
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Burenin, R.
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Burigana, C.
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Butler, R. C.
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Cardoso, J. -F.
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Carvalho, P.
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Catalano, A.
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Challinor, A.
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Chamballu, A.
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Chary, R. -R.
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Chiang, L. -Y.
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Chiang, H. C.
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Chon, G.
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Christensen, P. R.
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Church, S.
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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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Couchot, F.
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Coulais, A.
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Crill, B. P.
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Curto, A.
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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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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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Delouis, J. -M.
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Démoclès, 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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Dolag, K.
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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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Efstathiou, G.
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Enßlin, T. A.
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Eriksen, H. K.
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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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Hansen, F. K.
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Hanson, D.
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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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Hornstrup, A.
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Hovest, W.
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Huffenberger, K. M.
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Hurier, G.
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Jaffe, T. R.
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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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Khamitov, I.
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Kisner, T. S.
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Kneissl, R.
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Knoche, J.
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Knox, L.
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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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Laureijs, R. J.
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Lawrence, C. R.
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Leahy, J. P.
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Leonardi, R.
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León-Tavares, J.
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Lesgourgues, J.
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Liddle, A.
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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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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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Marcos-Caballero, A.
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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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Matthai, F.
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Mazzotta, P.
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Meinhold, P. R.
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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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Migliaccio, M.
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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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Moss, A.
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Munshi, D.
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Naselsky, P.
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Nati, F.
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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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Osborne, S.
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Oxborrow, C. A.
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Paci, F.
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Pagano, L.
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Pajot, F.
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Paoletti, D.
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Partridge, B.
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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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Pietrobon, D.
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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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Popa, L.
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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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Rachen, J. P.
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Rebolo, R.
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Reinecke, M.
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Remazeilles, 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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Roman, M.
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Rosset, C.
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Roudier, G.
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Rowan-Robinson, M.
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Rubiño-Martín, J. A.
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Rusholme, B.
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Sandri, M.
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Santos, D.
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Savini, G.
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Scott, D.
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Seiffert, M. D.
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Shellard, E. P. S.
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Spencer, L. D.
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Starck, J. -L.
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Stolyarov, V.
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Stompor, R.
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Sudiwala, R.
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Sunyaev, R.
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Sureau, F.
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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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Tavagnacco, D.
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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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Tuovinen, J.
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Türler, 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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Vittorio, N.
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Wade, L. A.
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Wandelt, B. D.
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Weller, J.
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White, M.
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White, S. D. 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 constraints on cosmological parameters using number counts as a function of redshift for a sub-sample of 189 galaxy clusters from the Planck SZ (PSZ) catalogue. The PSZ is selected through the signature of the Sunyaev-Zeldovich (SZ) effect, and the sub-sample used here has a signal-to-noise threshold of seven, with each object confirmed as a cluster and all but one with a redshift estimate. We discuss the completeness of the sample and our construction of a likelihood analysis. Using a relation between mass M and SZ signal Y calibrated to X-ray measurements, we derive constraints on the power spectrum amplitude σ8 and matter density parameter Ωm in a flat ΛCDM model. We test the robustness of our estimates and find that possible biases in the Y-M relation and the halo mass function are larger than the statistical uncertainties from the cluster sample. Assuming the X-ray determined mass to be biased low relative to the true mass by between zero and 30%, motivated by comparison of the observed mass scaling relations to those from a set of numerical simulations, we find that σ8 = 0.75 ± 0.03, Ωm = 0.29 ± 0.02, and σ8(Ωm/ 0.27)0.3 = 0.764 ± 0.025. The value of σ8 is degenerate with the mass bias; if the latter is fixed to a value of 20% (the central value from numerical simulations) we find σ8(Ωm/0.27)0.3 = 0.78 ± 0.01 and a tighter one-dimensional range σ8 = 0.77 ± 0.02. We find that the larger values of σ8 and Ωm preferred by Planck’s measurements of the primary CMB anisotropies can be accommodated by a mass bias of about 40%. Alternatively, consistency with the primary CMB constraints can be achieved by inclusion of processes that suppress power on small scales relative to the ΛCDM model, such as a component of massive neutrinos. We place our results in the context of other determinations of cosmologicalparameters, and discuss issues that need to be resolved in order to make further progress in this field.
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