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Centro de Astrofísica da Universidade do Porto

Planck Intermediate Results II: Comparison of Sunyaev-Zeldovich measurements from Planck and from the Arcminute Microkelvin Imager for 11 galaxy clusters

N. Aghanim, M. Arnaud, M. Ashdown, J. Aumont, C. Baccigalupi, A. Balbi, A. J. Banday, R. B. Barreiro, E. Battaner, R. Battye, K. Benabed, A. Benoît, J.-P. Bernard, M. Bersanelli, R. Bhatia, I. Bikmaev, H. Böhringer, A. Bonaldi, J. R. Bond, J. Borrill, F. R. Bouchet, H. Bourdin, M. L. Brown, M. Bucher, R. Burenin, C. Burigana, R. C. Butler, P. Cabella, P. Carvalho, A. Catalano, L. Cayón, A. Chamballu, R.-R. Chary, L.-Y. Chiang, G. Chon, D. L. Clements, S. Colafrancesco, S. Colombi, B. P. Crill, F. Cuttaia, A. C. da Silva, H. Dahle, R. D. Davies, R. J. Davis, P. de Bernardis, G. de Gasperis, A. de Rosa, G. de Zotti, J. Delabrouille, J. Démoclès, C. Dickinson, J. M. Diego, K. Dolag, H. Dole, S. Donzelli, O. Doré, M. Douspis, X. Dupac, T. A. Enβlin, H. K. Eriksen, F. Feroz, F. Finelli, I. Flores-Cacho, O. Forni, P. Fosalba, M. Frailis, E. Franceschi, S. Fromenteau, S. Galeotta, K. Ganga, R. T. Génova-Santos, M. Giard, Y. Giraud-Héraud, J. González-Nuevo, K. Górski, K. Grainge, A. Gregorio, A. Gruppuso, F. K. Hansen, D. L. Harrison, S. Henrot-Versillé, C. Hernández-Monteagudo, D. Herranz, S. R. Hildebrandt, E. Hivon, M. Hobson, W. A. Holmes, K. M. Huffenberger, G. Hurier, N. Hurley-Walker, T. Jagemann, M. Juvela, E. Keihänen, I. Khamitov, R. Kneissl, J. Knoche, M. Kunz, H. Kurki-Suonio, G. Lagache, J.-M. Lamarre, A. Lasenby, C. R. Lawrence, M. Le Jeune, S. Leach, R. Leonardi, A. Liddle, P. B. Lilje, M. Linden-Vørnle, M. López-Caniego, G. Luzzi, J. F. Macías-Pérez, C. J. MacTavish, D. Maino, N. Mandolesi, M. Maris, F. Marleau, D. J. Marshall, E. Martínez-González, S. Masi, M. Massardi, S. Matarrese, F. Matthai, P. Mazzotta, A. Melchiorri, J.-B. Melin, L. Mendes, A. Mennella, S. Mitra, M.-A. Miville-Deschênes, L. Montier, G. Morgante, D. Munshi, P. Naselsky, P. Natoli, F. Noviello, M. Olamaie, S. Osborne, F. Pajot, D. Paoletti, F. Pasian, G. Patanchon, T. J. Pearson, O. Perdereau, Y. Perrott, F. Perrotta, F. Piacentini, E. Pierpaoli, P. Platania, E. Pointecouteau, G. Polenta, L. Popa, T. Poutanen, G. W. Pratt, J.-L. Puget, J. P. Rachen, R. Rebolo López, M. Reinecke, M. Remazeilles, C. Renault, S. Ricciardi, I. Ristorcelli, G. Rocha, C. Rodríguez-Gonzálvez, C. Rosset, M. Rossetti, J. A. Rubiño-Martin, B. Rusholme, R. D. Saunders, G. Savini, M. P. Schammel, D. Scott, T. W. Shimwell, G. F. Smoot, J.-L. Starck, F. Stivoli, V. Stolyarov, R. Sunyaev, D. Sutton, A.-S. Suur-Uski, J.-F. Sygnet, J. A. Tauber, L. Terenzi, L. Toffolatti, M. Tomasi, M. Tristram, L. Valenziano, B. Van Tent, P. Vielva, F. Villa, N. Vittorio, L. A. Wade, B. D. Wandelt, D. Yvon, A. Zacchei, A. Zonca

A comparison is presented of Sunyaev–Zeldovich measurements for 11 galaxy clusters as obtained by Planck and by the ground-based interferometer, the ArcminuteMicrokelvin Imager. Assuming a universal spherically-symmetric Generalised Navarro, Frenk &White (GNFW)model for the cluster gas pressure profile, we jointly constrain the integrated Compton-Y parameter (Y500) and the scale radius (Θ500) of each cluster. Our resulting constraints in the Y500 - Θ500 2D parameter space derived from the two instruments overlap significantly for eight of the clusters, although, overall, there is a tendency for AMI to find the Sunyaev–Zeldovich signal to be smaller in angular size and fainter than Planck. Significant discrepancies exist for the three remaining clusters in the sample, namely A1413, A1914, and the newly-discovered Planck cluster PLCKESZ G139.59+24.18. The robustness of the analysis of both the Planck and AMI data is demonstrated through the use of detailed simulations, which also discount confusion from residual point (radio) sources and from diffuse astrophysical foregrounds as possible explanations for the discrepancies found. For a subset of our cluster sample, we have investigated the dependence of our results on the assumed pressure profile by repeating the analysis adopting the best-fitting GNFW profile shape which best matches X-ray observations. Adopting the best-fitting profile shape from the X-ray data does not, in general, resolve the discrepancies found in this subset of five clusters. Though based on a small sample, our results suggest that the adopted GNFW model may not be sufficiently flexible to describe clusters universally.

cosmology: observations – galaxies: clusters: general – galaxies: clusters: intracluster medium – cosmic background radiation – X-rays: galaxies: clusters

Astronomy and Astrophysics
Volume 550, Page A128_1
February 2013

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