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Astronomy and Astrophysics 550 (2013) A130
Planck Intermediate Results. IV. The XMM-Newton validation programme for new Planck galaxy clusters
P.A.R. Ade, N. Aghanim1, M. Arnaud, M. Ashdown, J. Aumont1, C. Baccigalupi, A. Balbi, A. J. Banday, R. B. Barreiro, J.G. Bartlett2, E. Battaner, K. Benabed, A. Benoit3, J.-P. Bernard, M. Bersanelli, I. Bikmaev, H. Böhringer, A. Bonaldi, J. R. Bond, S. Borgani, J. Borrill, F. R. Bouchet, M. L. Brown, C. Burigana, R. C. Butler, P. Cabella, P. Carvalho, A. Catalano4, L. Cayón, A. Chamballu, R.-R. Chary, L.-Y. Chiang, G. Chon, P. R. Christensen, D. L. Clements, S. Colafrancesco, S. Colombi, A. Coulais, B. P. Crill, F. Cuttaia, A. Da Silva, H. Dahle, R. J. Davis, P. De Bernardis, G. De Gasperis, G. de Zotti, J. Delabrouille2, J. Démoclès, F.-X. Désert, J. M. Diego, K. Dolag, H. Dole1, S. Donzelli, O. Doré, M. Douspis1, X. Dupac, T. A. Enßlin, H. K. Eriksen, F. Finelli, I. Flores-Cacho, O. Forni, M. Frailis, E. Franceschi, M. Frommert, S. Galeotta, K. Ganga2, R. T. Génova-Santos, Y. Giraud-Héraud2, J. González-Nuevo, R. González-Riestra, K. M. Górski, A. Gregorio, A. Gruppuso, F. K. Hansen, D. Harrison, A. Hempel, S. Henrot-Versillé, C. Hernández-Monteagudo, D. Herranz, S. R. Hildebrandt, E. Hivon, M. Hobson, W. A. Holmes, A. Hornstrup, W. Hovest, K. M. Huffenberger, G. Hurier4, A. H. Jaffe, T. Jagemann, W. C. Jones, M. Juvela, R. Kneissl, J. Knoche, L. Knox, M. Kunz1, H. Kurki-Suonio, G. Lagache1, J.-M. Lamarre, A. Lasenby, C. R. Lawrence, M. Le Jeune2, S. Leach, R. Leonardi, A. Liddle, P. B. Lilje, M. Linden-V\ornle, M. López-Caniego, G. Luzzi5, J.F. Macías-Pérez4, D. Maino, N. Mandolesi, R. Mann, M. Maris, F. Marleau, D. J. Marshall, E. Martínez-González, S. Masi, M. Massardi, S. Matarrese, P. Mazzotta, S. Mei, P. R. Meinhold, A. Melchiorri, J.-B. Melin, L. Mendes, A. Mennella, S. Mitra, M.-A. Miville-Deschênes1, A. Moneti, G. Morgante, D. Mortlock, D. Munshi, P. Naselsky, F. Nati, P. Natoli, H.U. Norgaard-Nielsen, F. Noviello1, S. Osborne, F. Pajot1, D. Paoletti, O. Perdereau5, F. Perrotta, F. Piacentini, M. Piat2, E. Pierpaoli, R. Piffaretti, S. Plaszczynski5, P. Platania, E. Pointecouteau, G. Polenta, L. Popa, T. Poutanen, G. W. Pratt, S. Prunet, J.-L. Puget1, M. Reinecke, M. Remazeilles1, 2, C. Renault4, S. Ricciardi, G. Rocha, C. Rosset2, M. Rossetti, J. A. Rubiño-Martín, B. Rusholme, M. Sandri, G. Savini, D. Scott, G.F. Smoot2, A. Stanford, F. Stivoli, R. Sudiwala, R. Sunyaev, D. Sutton, A.-S. Suur-Uski, J.-F. Sygnet, J. A. Tauber, L. Terenzi, L. Toffolatti, M. Tomasi, M. Tristram5, L. Valenziano, B. Van Tent6, P. Vielva, F. Villa, N. Vittorio, L. A. Wade, B. D. Wandelt, N. Welikala, J. Weller, S. D. M. White, D. Yvon, A. Zacchei, A. Zonca
For the PLANCK collaboration(s)
(2013-02)

We present the final results from the XMM-Newton validation follow-up of new Planck galaxy cluster candidates. We observed 15 new candidates, detected with signal-to-noise ratios between 4.0 and 6.1 in the 15.5-month nominal Planck survey. The candidates were selected using ancillary data flags derived from the ROSAT All Sky Survey (RASS) and Digitized Sky Survey all-sky maps, with the aim of pushing into the low SZ flux, high-z regime and testing RASS flags as indicators of candidate reliability. 14 new clusters were detected by XMM, including 2 double systems. Redshifts lie in the range 0.2 to 0.9, with 6 clusters at z>0.5. Estimated M500 range from 2.5 10^14 to 8 10^14 Msun. We discuss our results in the context of the full XMM validation programme, in which 51 new clusters have been detected. This includes 4 double and 2 triple systems, some of which are chance projections on the sky of clusters at different z. We find that association with a RASS-BSC source is a robust indicator of the reliability of a candidate, whereas association with a FSC source does not guarantee that the SZ candidate is a bona fide cluster. Nevertheless, most Planck clusters appear in RASS maps, with a significance greater than 2 sigma being a good indication that the candidate is a real cluster. The full sample gives a Planck sensitivity threshold of Y500 ~ 4 10^-4 arcmin^2, with indication for Malmquist bias in the YX-Y500 relation below this level. The corresponding mass threshold depends on z. Systems with M500 > 5 10^14 Msun at z > 0.5 are easily detectable with Planck. The newly-detected clusters follow the YX-Y500 relation derived from X-ray selected samples. Compared to X-ray selected clusters, the new SZ clusters have a lower X-ray luminosity on average for their mass. There is no indication of departure from standard self-similar evolution in the X-ray versus SZ scaling properties. (abridged)
1:  IAS - Institut d'astrophysique spatiale
2:  APC - UMR 7164 - AstroParticule et Cosmologie
3:  NEEL - Institut Néel
4:  LPSC - Laboratoire de Physique Subatomique et de Cosmologie
5:  LAL - Laboratoire de l'Accélérateur Linéaire
6:  LPT - Laboratoire de Physique Théorique d'Orsay [Orsay]
HELFA
APC - ADAMIS
APC - Cosmologie et Gravitation
Physics/Astrophysics/Cosmology and Extra-Galactic Astrophysics

Sciences of the Universe/Astrophysics/Cosmology and Extra-Galactic Astrophysics
Astrophysics - Cosmology and Extragalactic Astrophysics
Fulltext link: 
http://fr.arXiv.org/abs/1205.3376