Planck 2015 results XXIII. The thermal Sunyaev-Zeldovich effect-cosmic infrared background correlation

• Main Authors: Ade, PAR, Aghanim, N, Arnaud, M, Aumont, J, Baccigalupi, C, Banday, AJ, Barreiro, RB, Bartlett, JG, Bartolo, N, Battaner, E, Benabed, K, Benoit-Levy, A, Bernard, J-P, Bersanelli, M, Bielewicz, P, Bock, JJ, Bonaldi, A, Bonavera, L, Bond, JR, Borrill, J, Bouchet, FR, Burigana, C, Butler, RC, Calabrese, E, Catalano, A, Chamballu, A, Chiang, HC, Christensen, PR, Churazov, E, Clements, DL, Colombo, LPL, Combet, C, Comis, B, Couchot, F, Coulais, A, Crill, BP, Curto, A, Cuttaia, F, Danese, L, Davies, RD, Davis, RJ, de Bernardis, P, de Rosa, A, de Zotti, G, Delabrouille, J, Dickinson, C, Diego, JM, Dole, H, Donzelli, S, Dore, O, Douspis, M, Ducout, A, Dupac, X, Efstathiou, G, Elsner, F, Ensslin, TA, Eriksen, HK, Finelli, F, Flores-Cacho, I, Forni, O, Frailis, M, Fraisse, AA, Franceschi, E, Galeotta, S, Galli, S, Ganga, K, Genova-Santos, RT, Giard, M, Giraud-Heraud, Y, Gjerlow, E, Gonzalez-Nuevo, J, Gorski, KM, Gregorio, A, Gruppuso, A, Gudmundsson, JE, Hansen, FK, Harrison, DL, Helou, G, Hernandez-Monteagudo, C, Herranz, D, Hildebrandt, SR, Hivon, E, Hobson, M, Hornstrup, A, Hovest, W, Huffenberger, KM, Hurier, G, Jaffe, AH, Jaffe, TR, Jones, WC, Keihanen, E, Keskitalo, R, Kisner, TS, Kneissl, R, Knoche, J, Kunz, M, Kurki-Suonio, H, Lagache, G, Lamarre, J-M, Langer, M, Lasenby, A, Lattanzi, M, Lawrence, CR, Leonardi, R, Levrier, F, Lilje, PB, Linden-Vornle, M, Lopez-Caniego, M, Lubin, PM, Macias-Perez, JF, Maffei, B, Maggio, G, Maino, D, Mak, DSY, Mandolesi, N, Mangilli, A, Maris, M, Martin, PG, Martinez-Gonzalez, E, Masi, S, Matarrese, S, Melchiorri, A, Mennella, A, Migliaccio, M, Mitra, S, Miville-Deschenes, M-A, Moneti, A, Montier, L, Morgante, G, Mortlock, D, Munshi, D, Murphy, JA, Nati, F, Natoli, P, Noviello, F, Novikov, D, Novikov, I, Oxborrow, CA, Paci, F, Pagano, L, Pajot, F, Paoletti, D, Partridge, B, Pasian, F, Pearson, TJ, Perdereau, O, Perotto, L, Pettorino, V, Piacentini, F, Piat, M, Pierpaoli, E, Plaszczynski, S, Pointecouteau, E, Polenta, G, Ponthieu, N, Pratt, GW, Prunet, S, Puget, J-L, Rachen, JP, Reinecke, M, Remazeilles, M, Renault, C, Renzi, A, Ristorcelli, I, Rocha, G, Rosset, C, Rossetti, M, Roudier, G, Rubino-Martin, JA, Rusholme, B, Sandri, M, Santos, D, Savelainen, M, Savini, G, Scott, D, Spencer, LD, Stolyarov, V, Stompor, R, Sunyaev, R, Sutton, D, Suur-Uski, A-S, Sygnet, J-F, Tauber, JA, Terenzi, L, Toffolatti, L, Tomasi, M, Tristram, M, Tucci, M, Umana, G, Valenziano, L, Valiviita, J, Van Tent, B, Vielva, P, Villa, F, Wade, LA, Wandelt, BD, Wehus, IK, Welikala, N, Yvon, D, Zacchei, A, Zonca, A
• Format: Article in Journal/Newspaper
• Language: unknown
• Published: EDP SCIENCES S A 2016
• Subjects: Science & Technology; Physical Sciences; Astronomy & Astrophysics; galaxies: clusters: general; infrared: galaxies; large-scale structure of Universe; methods: data analysis; SOUTH-POLE TELESCOPE; ANGULAR POWER SPECTRUM; DARK-MATTER HALOES; GALAXY CLUSTERS; STAR-FORMATION; COSMOLOGICAL PARAMETERS; SUBMILLIMETER GALAXIES; SZ; ANISOTROPIES; MODEL; Navarro; South Pole; South pole
• Online Access: https://discovery.ucl.ac.uk/id/eprint/1542999/1/aa27418-15.pdf; https://discovery.ucl.ac.uk/id/eprint/1542999/

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.