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Aghanim, N;Arnaud, M;Ashdown, M;Aumont, J;Baccigalupi, C;Balbi, A;Banday, AJ;Barreiro, RB;Bartelmann, M;Bartlett, JG;Battaner, E;Benabed, K;Benoit, A;Bernard, JP;Bersanelli, M;Bhatia, R;Bock, JJ;Bonaldi, A;Bond, JR;Borrill, J;Bouchet, FR;Brown, ML;Bucher, M;Burigana, C;Cabella, P;Cardoso, JF;Catalano, A;Cayon, L;Challinor, A;Chamballu, A;Chiang, LY;Chiang, C;Chon, G;Christensen, PR;Churazov, E;Clements, DL;Colafrancesco, S;Colombi, S;Couchot, F;Coulais, A;Crill, BP;Cuttaia, F;Da Silva, A;Dahle, H;Danese, L;Davis, RJ;de Bernardis, P;de Gasperis, G;de Rosa, A;de Zotti, G;Delabrouille, J;Delouis, JM;Desert, FX;Diego, JM;Dolag, K;Donzelli, S;Dore, O;Dorl, U;Douspis, M;Dupac, X;Efstathiou, G;Ensslin, TA;Finelli, F;Flores-Cacho, I;Forni, O;Frailis, M;Franceschi, E;Fromenteau, S;Galeotta, S;Ganga, K;Genova-Santos, RT;Giard, M;Giardino, G;Giraud-Heraud, Y;Gonzalez-Nuevo, J;Gorski, KM;Gratton, S;Gregorio, A;Gruppuso, A;Harrison, D;Henrot-Versille, S;Hernandez-Monteagudo, C;Herranz, D;Hildebrandt, SR;Hivon, E;Hobson, M;Holmes, WA;Hovest, W;Hoyland, RJ;Huffenberger, KM;Jaffe, AH;Jones, WC;Juvela, M;Keihanen, E;Keskitalo, R;Kisner, TS;Kneissl, R;Knox, L;Kurki-Suonio, H;Lagache, G;Lamarre, JM;Lasenby, A;Laureijs, RJ;Lawrence, CR;Leach, S;Leonardi, R;Linden-Vornle, M;Lopez-Caniego, M;Lubin, PM;Macias-Perez, JF;MacTavish, CJ;Maffei, B;Maino, D;Mandolesi, N;Mann, R;Maris, M;Marleau, F;Martinez-Gonzalez, E;Masi, S;Matarrese, S;Matthai, F;Mazzotta, P;Mei, S;Melchiorri, A;Melin, JB;Mendes, L;Mennella, A;Mitra, S;Miville-Deschenes, MA;Moneti, A;Montier, L;Morgante, G;Mortlock, D;Munshi, D;Murphy, A;Naselsky, P;Natoli, P;Netterfield, CB;Norgaard-Nielsen, HU;Noviello, F;Novikov, D;Novikov, I;O'Dwyer, IJ;Osborne, S;Pajot, F;Pasian, F;Patanchon, G;Perdereau, O;Perotto, L;Perrotta, F;Piacentini, F;Piat, M;Pierpaoli, E;Piffaretti, R;Plaszczynski, S;Pointecouteau, E;Polenta, G;Ponthieu, N;Poutanen, T;Pratt, GW;Prezeau, G;Prunet, S;Puget, JL;Rebolo, R;Reinecke, M;Renault, C;Ricciardi, S;Riller, T;Ristorcelli, I;Rocha, G;Rosset, C;Rubino-Martin, JA;Rusholme, B;Sandri, M;Savini, G;Schaefer, BM;Scott, D;Seiffert, MD;Shellard, P;Smoot, GF;Starck, JL;Stivoli, F;Stolyarov, V;Sudiwala, R;Sunyaev, R;Sygnet, JF;Tauber, JA;Terenzi, L;Toffolatti, L;Tomasi, M;Torre, JP;Tristram, M;Tuovinen, J;Valenziano, L;Vibert, L;Vielva, P;Villa, F;Vittorio, N;Wandelt, BD;White, SDM;White, M;Yvon, D;Zacchei, A;Zonca, A
2011
December
Astronomy and Astrophysics
Planck early results. XII. Cluster Sunyaev-Zeldovich optical scaling relations
Published
83 ()
Optional Fields
SOUTH-POLE TELESCOPE DIGITAL SKY SURVEY PRE-LAUNCH STATUS GALAXY CLUSTERS RICHNESS RELATION L-X CATALOG COSMOLOGY MAXBCG SAMPLE
536
We present the Sunyaev-Zeldovich (SZ) signal-to-richness scaling relation (Y-500 - N-200) 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 (N-200 - M-500). We bin our individual measurements and detect the SZ signal down to the lowest richness systems (N-200 = 10) with high significance, achieving a detection of the SZ signal in systems with mass as low as M-500 approximate to 5 x 10(13) M-circle dot. The observed Y-500 - N-200 relation is well modeled by a power law over the full richness range. It has a lower normalisation at given N-200 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 Y-500 - N-200 relation of 60% rising to of order 100% at low richness. Thanks to its all-sky coverage, Planck provides observations for more than 13 000 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.
LES ULIS CEDEX A
0004-6361
10.1051/0004-6361/201116489
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