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Planck 2013 results. XIX. The integrated Sachs-Wolfe effect

Planck Collaboration, 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, N. Bartolo, E. Battaner, K. Benabed, A. Benoît, A. Benoit-Lévy, J. -P. Bernard, M. Bersanelli, P. Bielewicz, J. Bobin, J. J. Bock, A. Bonaldi, L. Bonavera, J. R. Bond, J. Borrill, F. R. Bouchet, M. Bridges, M. Bucher, C. Burigana, R. C. Butler, J. -F. Cardoso, A. Catalano, A. Challinor, A. Chamballu, 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. Désert, C. Dickinson, J. M. Diego, K. Dolag, H. Dole, S. Donzelli, O. Doré, M. Douspis, X. Dupac, G. Efstathiou, T. A. Enßlin, H. K. Eriksen, J. Fergusson, F. Finelli, O. Forni, P. Fosalba, M. Frailis, E. Franceschi, M. Frommert, S. Galeotta, K. Ganga, R. T. Génova-Santos, M. Giard, G. Giardino, Y. Giraud-Héraud, J. González-Nuevo, K. M. Górski, S. Gratton, A. Gregorio, A. Gruppuso, F. K. Hansen, D. Hanson, D. Harrison, S. Henrot-Versillé, C. Hernández-Monteagudo, D. Herranz, S. R. Hildebrandt, E. Hivon, S. Ho, M. Hobson, W. A. Holmes, A. Hornstrup, W. Hovest, K. M. Huffenberger, S. Ilić, A. H. Jaffe, T. R. Jaffe, J. Jasche, W. C. Jones, M. Juvela, E. Keihänen, R. Keskitalo, T. S. Kisner, J. Knoche, L. Knox, M. Kunz, H. Kurki-Suonio, G. Lagache, A. Lähteenmäki, J. -M. Lamarre, M. Langer, A. Lasenby, R. J. Laureijs, C. R. Lawrence, J. P. Leahy, R. Leonardi, J. Lesgourgues, M. Liguori, P. B. Lilje, M. Linden-Vørnle, M. López-Caniego, P. M. Lubin, J. F. Macías-Pérez, B. Maffei, D. Maino, N. Mandolesi, A. Mangilli, A. Marcos-Caballero, M. Maris, D. J. Marshall, P. G. Martin, E. Martínez-González, S. Masi, M. Massardi, S. Matarrese, F. Matthai, P. Mazzotta, P. R. Meinhold, A. Melchiorri, L. Mendes, A. Mennella, M. Migliaccio, S. Mitra, M. -A. Miville-Deschênes, A. Moneti, L. Montier, G. Morgante, D. Mortlock, A. Moss, D. Munshi, P. Naselsky, F. Nati, P. Natoli, C. B. Netterfield, H. U. Nørgaard-Nielsen, F. Noviello, D. Novikov, I. Novikov, S. Osborne, C. A. Oxborrow, F. Paci, L. Pagano, F. Pajot, 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. Prézeau, S. Prunet, J. -L. Puget, J. P. Rachen, B. Racine, R. Rebolo, M. Reinecke, M. Remazeilles, C. Renault, A. Renzi, S. Ricciardi, T. Riller, I. Ristorcelli, G. Rocha, C. Rosset, G. Roudier, M. Rowan-Robinson, J. A. Rubiño-Martín, B. Rusholme, M. Sandri, D. Santos, G. Savini, B. M. Schaefer, F. Schiavon, D. Scott, M. D. Seiffert, E. P. S. Shellard, L. D. Spencer, J. -L. Starck, V. Stolyarov, R. Stompor, R. Sudiwala, R. Sunyaev, F. Sureau, P. Sutter, 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, G. Umana, L. Valenziano, J. Valiviita, B. Van Tent, J. Varis, M. Viel, P. Vielva, F. Villa, N. Vittorio, L. A. Wade, B. D. Wandelt, M. White, J. -Q. Xia, D. Yvon, A. Zacchei, A. Zonca

TL;DR

This paper presents Planck 2013 results on the integrated Sachs-Wolfe (ISW) effect, exploiting three complementary approaches: ISW–lensing bispectrum, cross-correlations with large-scale structure (NVSS, SDSS CMASS/LOWZ, and SDSS Main sample), and aperture photometry on superstructures. It also introduces an ISW map reconstruction using CMB data and LSS tracers. The ISW detections are around $2.5$–$3\sigma$ across methods, with the strongest signal from NVSS cross-correlations and notable consistency across component-separation maps, supporting a dark-energy–driven decay of gravitational potentials in a $\Lambda$CDM universe. While lensing-based ISW detection yields robust Planck-only evidence, some stacking analyses show tension in amplitude and scale with standard predictions, highlighting ongoing challenges in modelling superstructure contributions; overall, Planck confirms ISW as a viable probe of cosmic acceleration, and Planck’s full frequency coverage strengthens foreground control and achromaticity checks.

Abstract

Based on CMB maps from the 2013 Planck Mission data release, this paper presents the detection of the ISW effect, i.e., the correlation between the CMB and large-scale evolving gravitational potentials. The significance of detection ranges from 2 to 4 sigma, depending on which method is used. We investigate three separate approaches, which cover essentially all previous studies, as well as breaking new ground. (i) Correlation of the CMB with the Planck reconstructed gravitational lensing potential (for the first time). This detection is made using the lensing-induced bispectrum; the correlation between lensing and the ISW effect has a significance close to 2.5 sigma. (ii) Cross-correlation with tracers of LSS, yielding around 3 sigma significance, based on a combination of radio (NVSS) and optical (SDSS) data. (iii) Aperture photometry on stacked CMB fields at the locations of known large-scale structures, which yields a 4 sigma signal when using a previously explored catalogue, but shows strong discrepancies in amplitude and scale compared to expectations. More recent catalogues give more moderate results, ranging from negligible to 2.5 sigma at most, but with a more consistent scale and amplitude, the latter being still slightly above what is expected from numerical simulations within LCMD. Where they can be compared, these measurements are compatible with previous work using data from WMAP, which had already mapped these scales to the limits of cosmic variance. Planck's broader frequency coverage confirms that the signal is achromatic, bolstering the case for ISW detection. As a final step we use tracers of large-scale structure to filter the CMB data, presenting maps of the ISW temperature perturbation. These results provide complementary and independent evidence for the existence of a dark energy component that governs the current accelerated expansion of the Universe.

Planck 2013 results. XIX. The integrated Sachs-Wolfe effect

TL;DR

This paper presents Planck 2013 results on the integrated Sachs-Wolfe (ISW) effect, exploiting three complementary approaches: ISW–lensing bispectrum, cross-correlations with large-scale structure (NVSS, SDSS CMASS/LOWZ, and SDSS Main sample), and aperture photometry on superstructures. It also introduces an ISW map reconstruction using CMB data and LSS tracers. The ISW detections are around – across methods, with the strongest signal from NVSS cross-correlations and notable consistency across component-separation maps, supporting a dark-energy–driven decay of gravitational potentials in a CDM universe. While lensing-based ISW detection yields robust Planck-only evidence, some stacking analyses show tension in amplitude and scale with standard predictions, highlighting ongoing challenges in modelling superstructure contributions; overall, Planck confirms ISW as a viable probe of cosmic acceleration, and Planck’s full frequency coverage strengthens foreground control and achromaticity checks.

Abstract

Based on CMB maps from the 2013 Planck Mission data release, this paper presents the detection of the ISW effect, i.e., the correlation between the CMB and large-scale evolving gravitational potentials. The significance of detection ranges from 2 to 4 sigma, depending on which method is used. We investigate three separate approaches, which cover essentially all previous studies, as well as breaking new ground. (i) Correlation of the CMB with the Planck reconstructed gravitational lensing potential (for the first time). This detection is made using the lensing-induced bispectrum; the correlation between lensing and the ISW effect has a significance close to 2.5 sigma. (ii) Cross-correlation with tracers of LSS, yielding around 3 sigma significance, based on a combination of radio (NVSS) and optical (SDSS) data. (iii) Aperture photometry on stacked CMB fields at the locations of known large-scale structures, which yields a 4 sigma signal when using a previously explored catalogue, but shows strong discrepancies in amplitude and scale compared to expectations. More recent catalogues give more moderate results, ranging from negligible to 2.5 sigma at most, but with a more consistent scale and amplitude, the latter being still slightly above what is expected from numerical simulations within LCMD. Where they can be compared, these measurements are compatible with previous work using data from WMAP, which had already mapped these scales to the limits of cosmic variance. Planck's broader frequency coverage confirms that the signal is achromatic, bolstering the case for ISW detection. As a final step we use tracers of large-scale structure to filter the CMB data, presenting maps of the ISW temperature perturbation. These results provide complementary and independent evidence for the existence of a dark energy component that governs the current accelerated expansion of the Universe.

Paper Structure

This paper contains 32 sections, 50 equations, 11 figures, 7 tables.

Table of Contents

  1. Introduction
  2. Data description
  3. Planck data
  4. CMB maps
  5. Lensing potential map
  6. External data sets
  7. NVSS radio catalogues
  8. SDSS luminous galaxies
  9. Main photometric SDSS galaxy sample
  10. SDSS, super-structures
  11. ISW-lensing bispectrum
  12. ISW-lensing estimators
  13. Lensing potential reconstruction
  14. KSW-estimator
  15. Binned bispectrum
  16. ...and 17 more sections

Figures (11)

  • Figure 1: Left: one of the CMB maps used in this paper, constructed using SEVEM (given at $N_\mathrm{side}$ = 64). Other Planck CMB maps used in this work are Commander-Ruler, NILC and SMICA, in addition to clean SEVEM maps from 44 to 353GHz. Right: Planck lensing map, optimally filtered to perform the ISW--lensing cross-correlation (given at $N_\mathrm{side}$ = 1024). See planck2013-p06 and planck2013-p12 for a detailed description of these maps.
  • Figure 2: Redshift distributions of the different surveys used in this work as LSS tracers, to be correlated with the Planck CMB maps. For ease of comparison, these distributions have been normalised to unity.
  • Figure 3: Density contrast maps obtained from the galaxy catalogues at $N_\mathrm{side}$ = 64. From top to bottom: NVSS; SDSS-CMASS/LOWZ; and SDSS-MphG.
  • Figure 4: Angular power spectra from the maps in Fig. \ref{['fig:surveys_maps']}. From top to bottom: NVSS; SDSS-CMASS/LOWZ; and SDSS-MphG. The observed spectra are the red points, whereas the theoretical models are represented by the black lines (the grey areas correspond to the sampling variance).
  • Figure 5: Observed and expected cross-correlation signal versus multipole $\ell$, for several surveys and different cross-correlation estimators. Columns from left to right correspond to: CAPS; CCF; and SMHWcov. Rows from top to bottom represent: NVSS; SDSS-CMASS/LOWZ; and SDSS-MphG. On each panel we show the expected cross-correlation (black line) and the $\pm1\sigma$ region (grey area).
  • ...and 6 more figures