{"paper":{"title":"Planck 2013 results. XXX. Cosmic infrared background measurements and implications for star formation","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.CO","authors_text":"A. Beno\\^it, A. Benoit-L\\'evy, A. Bonaldi, A. Catalano, A. Challinor, A. Chamballu, A. Coulais, A. Curto, A. De Rosa, A. Gregorio, A. Gruppuso, A. H. Jaffe, A. Hornstrup, A. J. Banday, A. L\\\"ahteenm\\\"aki, A. Lasenby, A. Melchiorri, A. Mennella, A. Moneti, A.-S. Suur-Uski, A. Zacchei, A. Zonca, B. D. Wandelt, B. Maffei, B. Partridge, B. P. Crill, B. Rusholme, B. Van Tent, B. Winkel, C. A. Oxborrow, C. Armitage-Caplan, C. Baccigalupi, C. B. Netterfield, C. Burigana, C. Dickinson, C. Hern\\'andez-Monteagudo, C. Renault, C. R. Lawrence, C. Rosset, D. Hanson, D. Harrison, D. Herranz, D. J. Marshall, D. L. Clements, D. Maino, D. Mortlock, D. Munshi, D. Novikov, D. Paoletti, D. Pietrobon, D. Santos, D. Scott, D. Sutton, D. Tavagnacco, D. Yvon, E. Battaner, E. Franceschi, E. Hivon, E. Keih\\\"anen, E. Mart\\'inez-Gonz\\'alez, E. Pierpaoli, E. Pointecouteau, E. P. S. Shellard, F. Atrio-Barandela, F. Boulanger, F. Couchot, F. Cuttaia, F. Finelli, F. K. Hansen, F. Lacasa, F. Matthai, F. Nati, F. Noviello, F. Paci, F. Pajot, F. Pasian, F. Perrotta, F. Piacentini, F. R. Bouchet, F. Sureau, F. Villa, F.-X. D\\'esert, G. de Zotti, G. Efstathiou, G. Helou, G. Lagache, G. Morgante, G. Patanchon, G. Polenta, G. Pr\\'ezeau, G. Rocha, G. Roudier, G. Savini, G. W. Pratt, H. C. Chiang, H. Dole, H. K. Eriksen, H. Kurki-Suonio, H. U. N{\\o}rgaard-Nielsen, I. Novikov, I. Ristorcelli, J. A. Murphy, J. A. Rubi\\~no-Mart\\'in, J. A. Tauber, J. Aumont, J. Bobin, J. Borrill, J. Delabrouille, J.-F. Cardoso, J. F. Mac\\'ias-P\\'erez, J.-F. Sygnet, J. G. Bartlett, J. Gonz\\'alez-Nuevo, J. J. Bock, J. Kerp, J. Knoche, J. Le\\'on-Tavares, J. Lesgourgues, J.-L. Puget, J.-L. Starck, J.-M. Delouis, J. M. Diego, J.-M. Lamarre, J.-P. Bernard, J. P. Rachen, J. R. Bond, J. Tuovinen, J. Valiviita, K. Benabed, K. Blagrave, K. Ganga, K. M. G\\'orski, K. M. Huffenberger, L. A. Wade, L. Danese, L. D. Spencer, L. Knox, L. Mendes, L. Montier, L. Pagano, L. Perotto, L. P. L. Colombo, L. Popa, L. Terenzi, L. Toffolatti, L. Valenziano, L.-Y Chiang, M.-A. Miville-Desch\\^enes, M. Arnaud, M. Ashdown, M. Bersanelli, M. Bethermin, M. Bridges, M. Bucher, M. Douspis, M. D. Seiffert, M. Frailis, M. Giard, M. Hobson, M. Juvela, M. Kunz, M. Langer, M. Liguori, M. Linden-V{\\o}rnle, M. L\\'opez-Caniego, M. Maris, M. Migliaccio, M. Piat, M. Reinecke, M. Remazeilles, M. Rowan-Robinson, M. Sandri, M. Tomasi, M. Tristram, M. Tucci, M. T\\\"urler, M. White, N. Aghanim, N. Mandolesi, N. Ponthieu, N. Vittorio, N. Welikala, O. Dor\\'e, O. Forni, O. Perdereau, P. Bielewicz, P. B. Lilje, P. De Bernardis, P. G. Martin, P. Kalberla, Planck Collaboration: P. A. R. Ade, P. Mazzotta, P. M. Lubin, P. Naselsky, P. Natoli, P. R. Christensen, P. Serra, P. Vielva, R. B. Barreiro, R. C. Butler, R. D. Davies, R. J. Davis, R. J. Laureijs, R. Keskitalo, R. Kneissl, R. Leonardi, R. Paladini, R. Rebolo, R. Stompor, R. Sudiwala, R. Sunyaev, S. Church, S. Colombi, S. D. M. White, S. Donzelli, S. Galeotta, S. Gratton, S. Henrot-Versill\\'e, S. Masi, S. Matarrese, S. Mitra, S. Osborne, S. Plaszczynski, S. Prunet, S. R. Hildebrandt, S. Ricciardi, T. A. En{\\ss}lin, T. Ghosh, T. Poutanen, T. Riller, T. R. Jaffe, T. S. Kisner, V. Stolyarov, W. A. Holmes, W. C. Jones, W. Hovest, W. T. Reach, X. Chen, X. Dupac, Y. Giraud-H\\'eraud","submitted_at":"2013-09-02T12:39:37Z","abstract_excerpt":"We present new measurements of CIB anisotropies using Planck. Combining HFI data with IRAS, the angular auto- and cross frequency power spectrum is measured from 143 to 3000 GHz, and the auto-bispectrum from 217 to 545 GHz. The total areas used to compute the CIB power spectrum and bispectrum are about 2240 and 4400 deg^2, respectively. After careful removal of the contaminants, and a complete study of systematics, the CIB power spectrum and bispectrum are measured with unprecedented signal to noise ratio from angular multipoles ell~150 to 2500, and ell~130 to 1100, respectively. Two approache"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1309.0382","kind":"arxiv","version":1},"verdict":{"id":null,"model_set":{},"created_at":null,"strongest_claim":"","one_line_summary":"","pipeline_version":null,"weakest_assumption":"","pith_extraction_headline":""},"references":{"count":0,"sample":[],"resolved_work":0,"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57","internal_anchors":0},"formal_canon":{"evidence_count":0,"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"author_claims":{"count":0,"strong_count":0,"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"builder_version":"pith-number-builder-2026-05-17-v1"}