September
2016
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2016A&A...594A..23P
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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Arnaud, M.
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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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Bartlett, J. G.
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Bartolo, N.
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Battaner, E.
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Benabed, K.
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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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Bock, J. J.
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Bonaldi, A.
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Bonavera, L.
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Bond, J. R.
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Borrill, J.
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Bouchet, F. R.
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Burigana, C.
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Butler, R. C.
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Calabrese, E.
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Catalano, A.
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Chamballu, A.
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Chiang, H. C.
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Christensen, P. R.
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Churazov, E.
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Clements, D. L.
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Colombo, L. P. L.
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Combet, C.
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Comis, B.
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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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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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Dickinson, C.
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Diego, J. M.
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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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Ducout, A.
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Dupac, X.
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Efstathiou, G.
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Elsner, F.
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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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Fraisse, A. A.
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Franceschi, E.
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Galeotta, S.
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Galli, 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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Giraud-Héraud, Y.
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Gjerløw, E.
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González-Nuevo, J.
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Górski, K. M.
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Gregorio, A.
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Gruppuso, A.
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Gudmundsson, J. E.
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Hansen, F. K.
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Harrison, D. L.
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Helou, G.
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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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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, A. H.
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Jaffe, T. R.
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Jones, W. C.
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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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Knoche, J.
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Kunz, M.
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Kurki-Suonio, H.
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Lagache, G.
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Lamarre, J. -M.
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Langer, M.
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Lasenby, A.
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Lattanzi, M.
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Lawrence, C. R.
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Leonardi, R.
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Levrier, F.
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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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Maggio, G.
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Maino, D.
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Mak, D. S. Y.
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Mandolesi, N.
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Mangilli, A.
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Maris, M.
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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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Melchiorri, A.
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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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Munshi, D.
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Murphy, J. A.
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Nati, F.
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Natoli, P.
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Noviello, F.
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Novikov, D.
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Novikov, I.
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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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Pearson, T. J.
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Perdereau, O.
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Perotto, L.
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Pettorino, V.
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Piacentini, F.
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Piat, M.
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Pierpaoli, E.
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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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Pratt, G. W.
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Prunet, S.
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Puget, J. -L.
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Rachen, J. P.
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Reinecke, M.
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Remazeilles, M.
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Renault, C.
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Renzi, A.
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Ristorcelli, I.
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Rocha, G.
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Rosset, C.
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Rossetti, M.
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Roudier, G.
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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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Savelainen, M.
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Savini, G.
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Scott, D.
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Spencer, L. D.
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Stolyarov, V.
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Stompor, R.
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Sunyaev, R.
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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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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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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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Wade, L. A.
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Wandelt, B. D.
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Wehus, I. K.
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Welikala, N.
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Yvon, D.
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Zacchei, A.
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Zonca, A.
Abstract
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We use Planck data to detect the cross-correlation between the thermal Sunyaev-Zeldovich (tSZ) effect and the infrared emission from the galaxies that make up the the cosmic infrared background (CIB). We first perform a stacking analysis towards Planck-confirmed galaxy clusters. We detect infrared emission produced by dusty galaxies inside these clusters and demonstrate that the infrared emission is about 50% more extended than the tSZ effect. Modelling the emission with a Navarro-Frenk-White profile, we find that the radial profile concentration parameter is c500 = 1.00+0.18-0.15 . This indicates that infrared galaxies in the outskirts of clusters have higher infrared flux than cluster-core galaxies. We also study the cross-correlation between tSZ and CIB anisotropies, following three alternative approaches based on power spectrum analyses: (I) using a catalogue of confirmed clusters detected in Planck data; (II) using an all-sky tSZ map built from Planck frequency maps; and (III) using cross-spectra between Planck frequency maps. With the three different methods, we detect the tSZ-CIB cross-power spectrum at significance levels of (I) 6σ; (II) 3σ; and (III) 4σ. We model the tSZ-CIB cross-correlation signature and compare predictions with the measurements. The amplitude of the cross-correlation relative to the fiducial model is AtSZ-CIB = 1.2 ± 0.3. This result is consistent with predictions for the tSZ-CIB cross-correlation assuming the best-fit cosmological model from Planck 2015 results along with the tSZ and CIB scaling relations.
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