Planck 2013 results. XXX. Cosmic infrared background measurements and implications for star formation

P. A. R. Ade, N. Aghanim, C. Armitage-Caplan, M. Arnaud, M. Ashdown, F. Atrio-Barandela, J. Aumont, C. Baccigalupi, A. J. Banday, R. B. Barreiro, J. G. Bartlett, E. Battaner, K. Benabed, A. Benoit, A. Benoit-Levy, J. -P. Bernard, M. Bersanelli, M. Bethermin, P. Bielewicz, K. Blagrave & 221 others J. Bobin, J. J. Bock, A. Bonaldi, J. R. Bond, J. Borrill, F. R. Bouchet, F. Boulanger, M. Bridges, M. Bucher, C. Burigana, R. C. Butler, J. F. Cardoso, A. Catalano, A. Challinor, A. Chamballu, X. Chen, H. C. Chiang, L. -Y Chiang, P. R. Christensen, S. Church, D. L. Clements, S. Colombi, L. P. L. Colombo, F. Couchot, A. Coulais, B. P. Crill, A. Curto, F. Cuttaia, L. Danese, R. D. Davies, R. J. Davis, P. de Bernardis, A. de Rosa, G. de Zotti, J. Delabrouille, J. -M. Delouis, F. -X. Desert, C. Dickinson, J. M. Diego, H. Dole, S. Donzelli, O. Dore, M. Douspis, X. Dupac, G. Efstathiou, T. A. Ensslin, H. K. Eriksen, F. Finelli, O. Forni, M. Frailis, E. Franceschi, S. Galeotta, K. Ganga, T. Ghosh, M. Giard, Y. Giraud-Heraud, J. Gonzalez-Nuevo, K. M. Gorski, S. Gratton, A. Gregorio, A. Gruppuso, F. K. Hansen, D. Hanson, D. Harrison, G. Helou, S. Henrot-Versille, C. Hernandez-Monteagudo, D. Herranz, S. R. Hildebrandt, E. Hivon, M. Hobson, W. A. Holmes, Allan Hornstrup, W. Hovest, K. M. Huffenberger, A. H. Jaffe, T. R. Jaffe, W. C. Jones, M. Juvela, P. Kalberla, E. Keihanen, J. Kerp, R. Keskitalo, T. S. Kisner, R. Kneissl, J. Knoche, L. Knox, M. Kunz, H. Kurki-Suonio, F. Lacasa, G. Lagache, A. Lahteenmaki, J. -M. Lamarre, M. Langer, A. Lasenby, R. J. Laureijs, C. R. Lawrence, R. Leonardi, J. Leon-Tavares, J. Lesgourgues, M. Liguori, P. B. Lilje, Michael Linden-Vørnle, M. Lopez-Caniego, P. M. Lubin, J. F. Macias-Perez, B. Maffei, D. Maino, N. Mandolesi, M. Maris, D. J. Marshall, P. G. Martin, E. Martinez-Gonzalez, S. Masi, M. Massardi, S. Matarrese, F. Matthai, P. Mazzotta, A. Melchiorri, L. Mendes, A. Mennella, M. Migliaccio, S. Mitra, M. A. Miville-Deschenes, A. Moneti, L. Montier, G. Morgante, D. Mortlock, D. Munshi, J. A. Murphy, P. Naselsky, F. Nati, P. Natoli, C. B. Netterfield, Hans Ulrik Nørgaard-Nielsen, F. Noviello, D. Novikov, I. Novikov, S. Osborne, Carol Anne Oxborrow, F. Paci, L. Pagano, Fernand Pajot, R. Paladini, D. Paoletti, B. Partridge, F. Pasian, G. Patanchon, O. Perdereau, L. Perotto, F. Perrotta, F. Piacentini, M. Piat, E. Pierpaoli, D. Pietrobon, S. Plaszczynski, E. Pointecouteau, G. Polenta, N. Ponthieu, L. Popa, T. Poutanen, G. W. Pratt, G. Prezeau, S. Prunet, J. -L. Puget, J. P. Rachen, W. T. Reach, R. Rebolo, M. Reinecke, M. Remazeilles, C. Renault, S. Ricciardi, T. Riller, I. Ristorcelli, G. Rocha, C. Rosset, G. Roudier, M. Rowan-Robinson, J. A. Rubino-Martin, B. Rusholme, M. Sandri, D. Santos, G. Savini, D. Scott, M. D. Seiffert, P. Serra, E. P. S. Shellard, L. D. Spencer, J. -L. Starck, V. Stolyarov, R. Stompor, R. Sudiwala, R. Sunyaev, F. Sureau, D. Sutton, A. -S. Suur-Uski, J. -F. Sygnet, J. A. Tauber, D. Tavagnacco, L. Terenzi, L. Toffolatti, M. Tomasi, M. Tristram, M. Tucci, J. Tuovinen, M. Tuerler, L. Valenziano, J. Valiviita, B. Van Tent, P. Vielva, F. Villa, N. Vittorio, L. A. Wade, B. D. Wandelt, N. Welikala, M. White, S. D. M. White, B. Winkel, D. Yvon, A. Zacchei, A. Zonca

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Abstract

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 deg2, 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∫ ∼150 to 2500. The bispectrum due to the clustering of dusty, star-forming galaxies is measured from ∫ ∼ 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 (Meff/ MΘ) = 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.
Original languageEnglish
Article numberA30
JournalAstronomy & Astrophysics
Volume571
Number of pages39
ISSN0004-6361
DOIs
Publication statusPublished - 2014

Keywords

  • osmology: observations
  • arge-scale structure of Universe
  • Galaxies: star formation
  • Infrared: diffuse background

Cite this

Ade, P. A. R., Aghanim, N., Armitage-Caplan, C., Arnaud, M., Ashdown, M., Atrio-Barandela, F., ... Zonca, A. (2014). Planck 2013 results. XXX. Cosmic infrared background measurements and implications for star formation. Astronomy & Astrophysics, 571, [A30]. https://doi.org/10.1051/0004-6361/201322093
Ade, P. A. R. ; Aghanim, N. ; Armitage-Caplan, C. ; Arnaud, M. ; Ashdown, M. ; Atrio-Barandela, F. ; Aumont, J. ; Baccigalupi, C. ; Banday, A. J. ; Barreiro, R. B. ; Bartlett, J. G. ; Battaner, E. ; Benabed, K. ; Benoit, A. ; Benoit-Levy, A. ; Bernard, J. -P. ; Bersanelli, M. ; Bethermin, M. ; Bielewicz, P. ; Blagrave, K. ; Bobin, J. ; Bock, J. J. ; Bonaldi, A. ; Bond, J. R. ; Borrill, J. ; Bouchet, F. R. ; Boulanger, F. ; Bridges, M. ; Bucher, M. ; Burigana, C. ; Butler, R. C. ; Cardoso, J. F. ; Catalano, A. ; Challinor, A. ; Chamballu, A. ; Chen, X. ; Chiang, H. C. ; Chiang, L. -Y ; Christensen, P. R. ; Church, S. ; Clements, D. L. ; Colombi, S. ; Colombo, L. P. L. ; Couchot, F. ; Coulais, A. ; Crill, B. P. ; Curto, A. ; Cuttaia, F. ; Danese, L. ; Davies, R. D. ; Davis, R. J. ; de Bernardis, P. ; de Rosa, A. ; de Zotti, G. ; Delabrouille, J. ; Delouis, J. -M. ; Desert, F. -X. ; Dickinson, C. ; Diego, J. M. ; Dole, H. ; Donzelli, S. ; Dore, O. ; Douspis, M. ; Dupac, X. ; Efstathiou, G. ; Ensslin, T. A. ; Eriksen, H. K. ; Finelli, F. ; Forni, O. ; Frailis, M. ; Franceschi, E. ; Galeotta, S. ; Ganga, K. ; Ghosh, T. ; Giard, M. ; Giraud-Heraud, Y. ; Gonzalez-Nuevo, J. ; Gorski, K. M. ; Gratton, S. ; Gregorio, A. ; Gruppuso, A. ; Hansen, F. K. ; Hanson, D. ; Harrison, D. ; Helou, G. ; Henrot-Versille, S. ; Hernandez-Monteagudo, C. ; Herranz, D. ; Hildebrandt, S. R. ; Hivon, E. ; Hobson, M. ; Holmes, W. A. ; Hornstrup, Allan ; Hovest, W. ; Huffenberger, K. M. ; Jaffe, A. H. ; Jaffe, T. R. ; Jones, W. C. ; Juvela, M. ; Kalberla, P. ; Keihanen, E. ; Kerp, J. ; Keskitalo, R. ; Kisner, T. S. ; Kneissl, R. ; Knoche, J. ; Knox, L. ; Kunz, M. ; Kurki-Suonio, H. ; Lacasa, F. ; Lagache, G. ; Lahteenmaki, A. ; Lamarre, J. -M. ; Langer, M. ; Lasenby, A. ; Laureijs, R. J. ; Lawrence, C. R. ; Leonardi, R. ; Leon-Tavares, J. ; Lesgourgues, J. ; Liguori, M. ; Lilje, P. B. ; Linden-Vørnle, Michael ; Lopez-Caniego, M. ; Lubin, P. M. ; Macias-Perez, J. F. ; Maffei, B. ; Maino, D. ; Mandolesi, N. ; Maris, M. ; Marshall, D. J. ; Martin, P. G. ; 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, M. A. ; Moneti, A. ; Montier, L. ; Morgante, G. ; Mortlock, D. ; Munshi, D. ; Murphy, J. A. ; Naselsky, P. ; Nati, F. ; Natoli, P. ; Netterfield, C. B. ; Nørgaard-Nielsen, Hans Ulrik ; Noviello, F. ; Novikov, D. ; Novikov, I. ; Osborne, S. ; Oxborrow, Carol Anne ; Paci, F. ; Pagano, L. ; Pajot, Fernand ; 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, G. W. ; Prezeau, G. ; Prunet, S. ; Puget, J. -L. ; Rachen, J. P. ; Reach, W. T. ; 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, J. A. ; Rusholme, B. ; Sandri, M. ; Santos, D. ; Savini, G. ; Scott, D. ; Seiffert, M. D. ; Serra, P. ; Shellard, E. P. S. ; Spencer, L. D. ; Starck, J. -L. ; Stolyarov, V. ; Stompor, R. ; Sudiwala, R. ; Sunyaev, R. ; Sureau, F. ; Sutton, D. ; Suur-Uski, A. -S. ; Sygnet, J. -F. ; Tauber, J. A. ; Tavagnacco, D. ; Terenzi, L. ; Toffolatti, L. ; Tomasi, M. ; Tristram, M. ; Tucci, M. ; Tuovinen, J. ; Tuerler, M. ; Valenziano, L. ; Valiviita, J. ; Van Tent, B. ; Vielva, P. ; Villa, F. ; Vittorio, N. ; Wade, L. A. ; Wandelt, B. D. ; Welikala, N. ; White, M. ; White, S. D. M. ; Winkel, B. ; Yvon, D. ; Zacchei, A. ; Zonca, A. / Planck 2013 results. XXX. Cosmic infrared background measurements and implications for star formation. In: Astronomy & Astrophysics. 2014 ; Vol. 571.
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title = "Planck 2013 results. XXX. Cosmic infrared background measurements and implications for star formation",
abstract = "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 deg2, 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∫ ∼150 to 2500. The bispectrum due to the clustering of dusty, star-forming galaxies is measured from ∫ ∼ 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 (Meff/ MΘ) = 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.",
keywords = "osmology: observations, arge-scale structure of Universe, Galaxies: star formation, Infrared: diffuse background",
author = "Ade, {P. A. R.} and N. Aghanim and C. Armitage-Caplan and M. Arnaud and M. Ashdown and F. Atrio-Barandela and J. Aumont and C. Baccigalupi and Banday, {A. J.} and Barreiro, {R. B.} and Bartlett, {J. G.} and E. Battaner and K. Benabed and A. Benoit and A. Benoit-Levy and Bernard, {J. -P.} and M. Bersanelli and M. Bethermin and P. Bielewicz and K. Blagrave and J. Bobin and Bock, {J. J.} and A. Bonaldi and Bond, {J. R.} and J. Borrill and Bouchet, {F. R.} and F. Boulanger and M. Bridges and M. Bucher and C. Burigana and Butler, {R. C.} and Cardoso, {J. F.} and A. Catalano and A. Challinor and A. Chamballu and X. Chen and Chiang, {H. C.} and Chiang, {L. -Y} and Christensen, {P. R.} and S. Church and Clements, {D. L.} and S. Colombi and Colombo, {L. P. L.} and F. Couchot and A. Coulais and Crill, {B. P.} and A. Curto and F. Cuttaia and L. Danese and Davies, {R. D.} and Davis, {R. J.} and {de Bernardis}, P. and {de Rosa}, A. and {de Zotti}, G. and J. Delabrouille and Delouis, {J. -M.} and Desert, {F. -X.} and C. Dickinson and Diego, {J. M.} and H. Dole and S. Donzelli and O. Dore and M. Douspis and X. Dupac and G. Efstathiou and Ensslin, {T. A.} and Eriksen, {H. K.} and F. Finelli and O. Forni and M. Frailis and E. Franceschi and S. Galeotta and K. Ganga and T. Ghosh and M. Giard and Y. Giraud-Heraud and J. Gonzalez-Nuevo and Gorski, {K. M.} and S. Gratton and A. Gregorio and A. Gruppuso and Hansen, {F. K.} and D. Hanson and D. Harrison and G. Helou and S. Henrot-Versille and C. Hernandez-Monteagudo and D. Herranz and Hildebrandt, {S. R.} and E. Hivon and M. Hobson and Holmes, {W. A.} and Allan Hornstrup and W. Hovest and Huffenberger, {K. M.} and Jaffe, {A. H.} and Jaffe, {T. R.} and Jones, {W. C.} and M. Juvela and P. Kalberla and E. Keihanen and J. Kerp and R. Keskitalo and Kisner, {T. S.} and R. Kneissl and J. Knoche and L. Knox and M. Kunz and H. Kurki-Suonio and F. Lacasa and G. Lagache and A. Lahteenmaki and Lamarre, {J. -M.} and M. Langer and A. Lasenby and Laureijs, {R. J.} and Lawrence, {C. R.} and R. Leonardi and J. Leon-Tavares and J. Lesgourgues and M. Liguori and Lilje, {P. B.} and Michael Linden-V{\o}rnle and M. Lopez-Caniego and Lubin, {P. M.} and Macias-Perez, {J. F.} and B. Maffei and D. Maino and N. Mandolesi and M. Maris and Marshall, {D. J.} and Martin, {P. G.} and E. Martinez-Gonzalez and S. Masi and M. Massardi and S. Matarrese and F. Matthai and P. Mazzotta and A. Melchiorri and L. Mendes and A. Mennella and M. Migliaccio and S. Mitra and Miville-Deschenes, {M. A.} and A. Moneti and L. Montier and G. Morgante and D. Mortlock and D. Munshi and Murphy, {J. A.} and P. Naselsky and F. Nati and P. Natoli and Netterfield, {C. B.} and N{\o}rgaard-Nielsen, {Hans Ulrik} and F. Noviello and D. Novikov and I. Novikov and S. Osborne and Oxborrow, {Carol Anne} and F. Paci and L. Pagano and Fernand Pajot and R. Paladini and D. Paoletti and B. Partridge and F. Pasian and G. Patanchon and O. Perdereau and L. Perotto and F. Perrotta and F. Piacentini and M. Piat and E. Pierpaoli and D. Pietrobon and S. Plaszczynski and E. Pointecouteau and G. Polenta and N. Ponthieu and L. Popa and T. Poutanen and Pratt, {G. W.} and G. Prezeau and S. Prunet and Puget, {J. -L.} and Rachen, {J. P.} and Reach, {W. T.} and R. Rebolo and M. Reinecke and M. Remazeilles and C. Renault and S. Ricciardi and T. Riller and I. Ristorcelli and G. Rocha and C. Rosset and G. Roudier and M. Rowan-Robinson and Rubino-Martin, {J. A.} and B. Rusholme and M. Sandri and D. Santos and G. Savini and D. Scott and Seiffert, {M. D.} and P. Serra and Shellard, {E. P. S.} and Spencer, {L. D.} and Starck, {J. -L.} and V. Stolyarov and R. Stompor and R. Sudiwala and R. Sunyaev and F. Sureau and D. Sutton and Suur-Uski, {A. -S.} and Sygnet, {J. -F.} and Tauber, {J. A.} and D. Tavagnacco and L. Terenzi and L. Toffolatti and M. Tomasi and M. Tristram and M. Tucci and J. Tuovinen and M. Tuerler and L. Valenziano and J. Valiviita and {Van Tent}, B. and P. Vielva and F. Villa and N. Vittorio and Wade, {L. A.} and Wandelt, {B. D.} and N. Welikala and M. White and White, {S. D. M.} and B. Winkel and D. Yvon and A. Zacchei and A. Zonca",
year = "2014",
doi = "10.1051/0004-6361/201322093",
language = "English",
volume = "571",
journal = "Astronomy & Astrophysics",
issn = "0004-6361",
publisher = "E D P Sciences",

}

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, J-P, 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, L-Y, 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, J-M, Desert, F-X, 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, J-M, Langer, M, Lasenby, A, Laureijs, RJ, Lawrence, CR, Leonardi, R, Leon-Tavares, J, Lesgourgues, J, Liguori, M, Lilje, PB, Linden-Vørnle, 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, Nørgaard-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, J-L, 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, J-L, Stolyarov, V, Stompor, R, Sudiwala, R, Sunyaev, R, Sureau, F, Sutton, D, Suur-Uski, A-S, Sygnet, J-F, Tauber, JA, Tavagnacco, D, Terenzi, L, Toffolatti, L, Tomasi, M, Tristram, M, Tucci, M, Tuovinen, J, Tuerler, 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 2014, 'Planck 2013 results. XXX. Cosmic infrared background measurements and implications for star formation', Astronomy & Astrophysics, vol. 571, A30. https://doi.org/10.1051/0004-6361/201322093

Planck 2013 results. XXX. Cosmic infrared background measurements and implications for star formation. / Ade, P. A. R.; Aghanim, N.; Armitage-Caplan, C.; Arnaud, M.; Ashdown, M.; Atrio-Barandela, F.; Aumont, J.; Baccigalupi, C.; Banday, A. J.; Barreiro, R. B.; Bartlett, J. G.; Battaner, E.; Benabed, K.; Benoit, A.; Benoit-Levy, A.; Bernard, J. -P.; Bersanelli, M.; Bethermin, M.; Bielewicz, P.; Blagrave, K.; Bobin, J.; Bock, J. J.; Bonaldi, A.; Bond, J. R.; Borrill, J.; Bouchet, F. R.; Boulanger, F.; Bridges, M.; Bucher, M.; Burigana, C.; Butler, R. C.; Cardoso, J. F.; Catalano, A.; Challinor, A.; Chamballu, A.; Chen, X.; Chiang, H. C.; Chiang, L. -Y; Christensen, P. R.; Church, S.; Clements, D. L.; Colombi, S.; Colombo, L. P. L.; Couchot, F.; Coulais, A.; Crill, B. P.; Curto, A.; Cuttaia, F.; Danese, L.; Davies, R. D.; Davis, R. J.; de Bernardis, P.; de Rosa, A.; de Zotti, G.; Delabrouille, J.; Delouis, J. -M.; Desert, F. -X.; Dickinson, C.; Diego, J. M.; Dole, H.; Donzelli, S.; Dore, O.; Douspis, M.; Dupac, X.; Efstathiou, G.; Ensslin, T. A.; Eriksen, H. K.; Finelli, F.; Forni, O.; Frailis, M.; Franceschi, E.; Galeotta, S.; Ganga, K.; Ghosh, T.; Giard, M.; Giraud-Heraud, Y.; Gonzalez-Nuevo, J.; Gorski, K. M.; Gratton, S.; Gregorio, A.; Gruppuso, A.; Hansen, F. K.; Hanson, D.; Harrison, D.; Helou, G.; Henrot-Versille, S.; Hernandez-Monteagudo, C.; Herranz, D.; Hildebrandt, S. R.; Hivon, E.; Hobson, M.; Holmes, W. A.; Hornstrup, Allan; Hovest, W.; Huffenberger, K. M.; Jaffe, A. H.; Jaffe, T. R.; Jones, W. C.; Juvela, M.; Kalberla, P.; Keihanen, E.; Kerp, J.; Keskitalo, R.; Kisner, T. S.; Kneissl, R.; Knoche, J.; Knox, L.; Kunz, M.; Kurki-Suonio, H.; Lacasa, F.; Lagache, G.; Lahteenmaki, A.; Lamarre, J. -M.; Langer, M.; Lasenby, A.; Laureijs, R. J.; Lawrence, C. R.; Leonardi, R.; Leon-Tavares, J.; Lesgourgues, J.; Liguori, M.; Lilje, P. B.; Linden-Vørnle, Michael; Lopez-Caniego, M.; Lubin, P. M.; Macias-Perez, J. F.; Maffei, B.; Maino, D.; Mandolesi, N.; Maris, M.; Marshall, D. J.; Martin, P. G.; 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, M. A.; Moneti, A.; Montier, L.; Morgante, G.; Mortlock, D.; Munshi, D.; Murphy, J. A.; Naselsky, P.; Nati, F.; Natoli, P.; Netterfield, C. B.; Nørgaard-Nielsen, Hans Ulrik; Noviello, F.; Novikov, D.; Novikov, I.; Osborne, S.; Oxborrow, Carol Anne; Paci, F.; Pagano, L.; Pajot, Fernand; 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, G. W.; Prezeau, G.; Prunet, S.; Puget, J. -L.; Rachen, J. P.; Reach, W. T.; 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, J. A.; Rusholme, B.; Sandri, M.; Santos, D.; Savini, G.; Scott, D.; Seiffert, M. D.; Serra, P.; Shellard, E. P. S.; Spencer, L. D.; Starck, J. -L.; Stolyarov, V.; Stompor, R.; Sudiwala, R.; Sunyaev, R.; Sureau, F.; Sutton, D.; Suur-Uski, A. -S.; Sygnet, J. -F.; Tauber, J. A.; Tavagnacco, D.; Terenzi, L.; Toffolatti, L.; Tomasi, M.; Tristram, M.; Tucci, M.; Tuovinen, J.; Tuerler, M.; Valenziano, L.; Valiviita, J.; Van Tent, B.; Vielva, P.; Villa, F.; Vittorio, N.; Wade, L. A.; Wandelt, B. D.; Welikala, N.; White, M.; White, S. D. M.; Winkel, B.; Yvon, D.; Zacchei, A.; Zonca, A.

In: Astronomy & Astrophysics, Vol. 571, A30, 2014.

Research output: Contribution to journalJournal articleResearchpeer-review

TY - JOUR

T1 - Planck 2013 results. XXX. Cosmic infrared background measurements and implications for star formation

AU - Ade, P. A. R.

AU - Aghanim, N.

AU - Armitage-Caplan, C.

AU - Arnaud, M.

AU - Ashdown, M.

AU - Atrio-Barandela, F.

AU - Aumont, J.

AU - Baccigalupi, C.

AU - Banday, A. J.

AU - Barreiro, R. B.

AU - Bartlett, J. G.

AU - Battaner, E.

AU - Benabed, K.

AU - Benoit, A.

AU - Benoit-Levy, A.

AU - Bernard, J. -P.

AU - Bersanelli, M.

AU - Bethermin, M.

AU - Bielewicz, P.

AU - Blagrave, K.

AU - Bobin, J.

AU - Bock, J. J.

AU - Bonaldi, A.

AU - Bond, J. R.

AU - Borrill, J.

AU - Bouchet, F. R.

AU - Boulanger, F.

AU - Bridges, M.

AU - Bucher, M.

AU - Burigana, C.

AU - Butler, R. C.

AU - Cardoso, J. F.

AU - Catalano, A.

AU - Challinor, A.

AU - Chamballu, A.

AU - Chen, X.

AU - Chiang, H. C.

AU - Chiang, L. -Y

AU - Christensen, P. R.

AU - Church, S.

AU - Clements, D. L.

AU - Colombi, S.

AU - Colombo, L. P. L.

AU - Couchot, F.

AU - Coulais, A.

AU - Crill, B. P.

AU - Curto, A.

AU - Cuttaia, F.

AU - Danese, L.

AU - Davies, R. D.

AU - Davis, R. J.

AU - de Bernardis, P.

AU - de Rosa, A.

AU - de Zotti, G.

AU - Delabrouille, J.

AU - Delouis, J. -M.

AU - Desert, F. -X.

AU - Dickinson, C.

AU - Diego, J. M.

AU - Dole, H.

AU - Donzelli, S.

AU - Dore, O.

AU - Douspis, M.

AU - Dupac, X.

AU - Efstathiou, G.

AU - Ensslin, T. A.

AU - Eriksen, H. K.

AU - Finelli, F.

AU - Forni, O.

AU - Frailis, M.

AU - Franceschi, E.

AU - Galeotta, S.

AU - Ganga, K.

AU - Ghosh, T.

AU - Giard, M.

AU - Giraud-Heraud, Y.

AU - Gonzalez-Nuevo, J.

AU - Gorski, K. M.

AU - Gratton, S.

AU - Gregorio, A.

AU - Gruppuso, A.

AU - Hansen, F. K.

AU - Hanson, D.

AU - Harrison, D.

AU - Helou, G.

AU - Henrot-Versille, S.

AU - Hernandez-Monteagudo, C.

AU - Herranz, D.

AU - Hildebrandt, S. R.

AU - Hivon, E.

AU - Hobson, M.

AU - Holmes, W. A.

AU - Hornstrup, Allan

AU - Hovest, W.

AU - Huffenberger, K. M.

AU - Jaffe, A. H.

AU - Jaffe, T. R.

AU - Jones, W. C.

AU - Juvela, M.

AU - Kalberla, P.

AU - Keihanen, E.

AU - Kerp, J.

AU - Keskitalo, R.

AU - Kisner, T. S.

AU - Kneissl, R.

AU - Knoche, J.

AU - Knox, L.

AU - Kunz, M.

AU - Kurki-Suonio, H.

AU - Lacasa, F.

AU - Lagache, G.

AU - Lahteenmaki, A.

AU - Lamarre, J. -M.

AU - Langer, M.

AU - Lasenby, A.

AU - Laureijs, R. J.

AU - Lawrence, C. R.

AU - Leonardi, R.

AU - Leon-Tavares, J.

AU - Lesgourgues, J.

AU - Liguori, M.

AU - Lilje, P. B.

AU - Linden-Vørnle, Michael

AU - Lopez-Caniego, M.

AU - Lubin, P. M.

AU - Macias-Perez, J. F.

AU - Maffei, B.

AU - Maino, D.

AU - Mandolesi, N.

AU - Maris, M.

AU - Marshall, D. J.

AU - Martin, P. G.

AU - Martinez-Gonzalez, E.

AU - Masi, S.

AU - Massardi, M.

AU - Matarrese, S.

AU - Matthai, F.

AU - Mazzotta, P.

AU - Melchiorri, A.

AU - Mendes, L.

AU - Mennella, A.

AU - Migliaccio, M.

AU - Mitra, S.

AU - Miville-Deschenes, M. A.

AU - Moneti, A.

AU - Montier, L.

AU - Morgante, G.

AU - Mortlock, D.

AU - Munshi, D.

AU - Murphy, J. A.

AU - Naselsky, P.

AU - Nati, F.

AU - Natoli, P.

AU - Netterfield, C. B.

AU - Nørgaard-Nielsen, Hans Ulrik

AU - Noviello, F.

AU - Novikov, D.

AU - Novikov, I.

AU - Osborne, S.

AU - Oxborrow, Carol Anne

AU - Paci, F.

AU - Pagano, L.

AU - Pajot, Fernand

AU - Paladini, R.

AU - Paoletti, D.

AU - Partridge, B.

AU - Pasian, F.

AU - Patanchon, G.

AU - Perdereau, O.

AU - Perotto, L.

AU - Perrotta, F.

AU - Piacentini, F.

AU - Piat, M.

AU - Pierpaoli, E.

AU - Pietrobon, D.

AU - Plaszczynski, S.

AU - Pointecouteau, E.

AU - Polenta, G.

AU - Ponthieu, N.

AU - Popa, L.

AU - Poutanen, T.

AU - Pratt, G. W.

AU - Prezeau, G.

AU - Prunet, S.

AU - Puget, J. -L.

AU - Rachen, J. P.

AU - Reach, W. T.

AU - Rebolo, R.

AU - Reinecke, M.

AU - Remazeilles, M.

AU - Renault, C.

AU - Ricciardi, S.

AU - Riller, T.

AU - Ristorcelli, I.

AU - Rocha, G.

AU - Rosset, C.

AU - Roudier, G.

AU - Rowan-Robinson, M.

AU - Rubino-Martin, J. A.

AU - Rusholme, B.

AU - Sandri, M.

AU - Santos, D.

AU - Savini, G.

AU - Scott, D.

AU - Seiffert, M. D.

AU - Serra, P.

AU - Shellard, E. P. S.

AU - Spencer, L. D.

AU - Starck, J. -L.

AU - Stolyarov, V.

AU - Stompor, R.

AU - Sudiwala, R.

AU - Sunyaev, R.

AU - Sureau, F.

AU - Sutton, D.

AU - Suur-Uski, A. -S.

AU - Sygnet, J. -F.

AU - Tauber, J. A.

AU - Tavagnacco, D.

AU - Terenzi, L.

AU - Toffolatti, L.

AU - Tomasi, M.

AU - Tristram, M.

AU - Tucci, M.

AU - Tuovinen, J.

AU - Tuerler, M.

AU - Valenziano, L.

AU - Valiviita, J.

AU - Van Tent, B.

AU - Vielva, P.

AU - Villa, F.

AU - Vittorio, N.

AU - Wade, L. A.

AU - Wandelt, B. D.

AU - Welikala, N.

AU - White, M.

AU - White, S. D. M.

AU - Winkel, B.

AU - Yvon, D.

AU - Zacchei, A.

AU - Zonca, A.

PY - 2014

Y1 - 2014

N2 - 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 deg2, 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∫ ∼150 to 2500. The bispectrum due to the clustering of dusty, star-forming galaxies is measured from ∫ ∼ 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 (Meff/ MΘ) = 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.

AB - 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 deg2, 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∫ ∼150 to 2500. The bispectrum due to the clustering of dusty, star-forming galaxies is measured from ∫ ∼ 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 (Meff/ MΘ) = 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.

KW - osmology: observations

KW - arge-scale structure of Universe

KW - Galaxies: star formation

KW - Infrared: diffuse background

U2 - 10.1051/0004-6361/201322093

DO - 10.1051/0004-6361/201322093

M3 - Journal article

VL - 571

JO - Astronomy & Astrophysics

JF - Astronomy & Astrophysics

SN - 0004-6361

M1 - A30

ER -