A1 Refereed original research article in a scientific journal
Planck 2013 results. XXX. Cosmic infrared background measurements and implications for star formation
Authors: Ade PAR, Aghanim N, Armitage-Caplan C, Arnaud M, Ashdown M, Atrio-Barandela F, Aumont J, Baccigalupi C, Banday AJ, Barreiro RB, Bartlett JG, Battaner E, Benabed K, Benoit A, Benoit-Levy A, Bernard JP, Bersanelli M, Bethermin M, Bielewicz P, Blagrave K, Bobin J, Bock JJ, Bonaldi A, Bond JR, Borrill J, Bouchet FR, Boulanger F, Bridges M, Bucher M, Burigana C, Butler RC, Cardoso JF, Catalano A, Challinor A, Chamballu A, Chen X, Chiang HC, Chiang LY, Christensen PR, Church S, Clements DL, Colombi S, Colombo LPL, 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, Delouis JM, Desert FX, Dickinson C, Diego JM, Dole H, Donzelli S, Dore O, Douspis M, Dupac X, Efstathiou G, Ensslin TA, Eriksen HK, Finelli F, Forni O, Frailis M, Franceschi E, Galeotta S, Ganga K, Ghosh T, Giard M, Giraud-Heraud Y, Gonzalez-Nuevo J, Gorski KM, Gratton S, Gregorio A, Gruppuso A, Hansen FK, Hanson D, Harrison D, Helou G, Henrot-Versille S, Hernandez-Monteagudo C, Herranz D, Hildebrandt SR, Hivon E, Hobson M, Holmes WA, Hornstrup A, Hovest W, Huffenberger KM, Jaffe AH, Jaffe TR, Jones WC, Juvela M, Kalberla P, Keihanen E, Kerp J, Keskitalo R, Kisner TS, Kneissl R, Knoche J, Knox L, Kunz M, Kurki-Suonio H, Lacasa F, Lagache G, Lahteenmaki A, Lamarre JM, Langer M, Lasenby A, Laureijs RJ, Lawrence CR, Leonardi R, Leon-Tavares J, Lesgourgues J, Liguori M, Lilje PB, Linden-Vornle M, Lopez-Caniego M, Lubin PM, Macias-Perez JF, Maffei B, Maino D, Mandolesi N, Maris M, Marshall DJ, Martin PG, Martinez-Gonzalez E, Masi S, Massardi M, Matarrese S, Matthai F, Mazzotta P, Melchiorri A, Mendes L, Mennella A, Migliaccio M, Mitra S, Miville-Deschenes MA, Moneti A, Montier L, Morgante G, Mortlock D, Munshi D, Murphy JA, Naselsky P, Nati F, Natoli P, Netterfield CB, Norgaard-Nielsen HU, Noviello F, Novikov D, Novikov I, Osborne S, Oxborrow CA, Paci F, Pagano L, Pajot F, Paladini R, Paoletti D, Partridge B, Pasian F, Patanchon G, Perdereau O, Perotto L, Perrotta F, Piacentini F, Piat M, Pierpaoli E, Pietrobon D, Plaszczynski S, Pointecouteau E, Polenta G, Ponthieu N, Popa L, Poutanen T, Pratt GW, Prezeau G, Prunet S, Puget JL, Rachen JP, Reach WT, Rebolo R, Reinecke M, Remazeilles M, Renault C, Ricciardi S, Riller T, Ristorcelli I, Rocha G, Rosset C, Roudier G, Rowan-Robinson M, Rubino-Martin JA, Rusholme B, Sandri M, Santos D, Savini G, Scott D, Seiffert MD, Serra P, Shellard EPS, Spencer LD, Starck JL, Stolyarov V, Stompor R, Sudiwala R, Sunyaev R, Sureau F, Sutton D, Suur-Uski AS, Sygnet JF, Tauber JA, Tavagnacco D, Terenzi L, Toffolatti L, Tomasi M, Tristram M, Tucci M, Tuovinen J, Turler M, Valenziano L, Valiviita J, Van Tent B, Vielva P, Villa F, Vittorio N, Wade LA, Wandelt BD, Welikala N, White M, White SDM, Winkel B, Yvon D, Zacchei A, Zonca A
Publisher: EDP SCIENCES S A
Publication year: 2014
Journal: Astronomy and Astrophysics
Journal name in source: ASTRONOMY & ASTROPHYSICS
Journal acronym: ASTRON ASTROPHYS
Article number: ARTN A30
Volume: 571
Number of pages: 39
ISSN: 0004-6361
DOI: https://doi.org/10.1051/0004-6361/201322093
We present new measurements of cosmic infrared background (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 (cosmic microwave background anisotropies, Galactic dust, and Sunyaev-Zeldovich emission), and a complete study of systematics, the CIB power spectrum is measured with unprecedented signal to noise ratio from angular multipoles l similar to 150 to 2500. The bispectrum due to the clustering of dusty, star-forming galaxies is measured from l similar to 130 to 1100, with a total signal to noise ratio of around 6, 19, and 29 at 217, 353, and 545 GHz, respectively. Two approaches are developed for modelling CIB power spectrum anisotropies. The first approach takes advantage of the unique measurements by Planck at large angular scales, and models only the linear part of the power spectrum, with a mean bias of dark matter haloes hosting dusty galaxies at a given redshift weighted by their contribution to the emissivities. The second approach is based on a model that associates star-forming galaxies with dark matter haloes and their subhaloes, using a parametrized relation between the dust-processed infrared luminosity and (sub-) halo mass. The two approaches simultaneously fit all auto-and cross-power spectra very well. We find that the star formation history is well constrained up to redshifts around 2, and agrees with recent estimates of the obscured star-formation density using Spitzer and Herschel. However, at higher redshift, the accuracy of the star formation history measurement is strongly degraded by the uncertainty in the spectral energy distribution of CIB galaxies. We also find that the mean halo mass which is most efficient at hosting star formation is log (M-eff/ M-circle dot) = 12.6 and that CIB galaxies have warmer temperatures as redshift increases. The CIB bispectrum is steeper than that expected from the power spectrum, although well fitted by a power law; this gives some information about the contribution of massive haloes to the CIB bispectrum. Finally, we show that the same halo occupation distribution can fit all power spectra simultaneously. The precise measurements enabled by Planck pose new challenges for the modelling of CIB anisotropies, indicating the power of using CIB anisotropies to understand the process of galaxy formation.
