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

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

doi:10.1051/0004-6361/201321526

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

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. BobinJ. 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

Research output: Contribution to journal › Article › Research › peer-review

37 Citations (Scopus)

Abstract

© 2014 ESO. Based on cosmic microwave background (CMB) maps from the 2013 Planck Mission data release, this paper presents the detection of the integrated Sachs-Wolfe (ISW) effect, that is, the correlation between the CMB and large-scale evolving gravitational potentials. The significance of detection ranges from 2 to 4σ, depending on which method is used. We investigated three separate approaches, which essentially cover all previous studies, and also break new ground. (i) We correlated the CMB with the Planck reconstructed gravitational lensing potential (for the first time). This detection was made using the lensing-induced bispectrum between the low-â.," and high-â.," temperature anisotropies; the correlation between lensing and the ISW effect has a significance close to 2.5σ. (ii) We cross-correlated with tracers of large-scale structure, which yielded a significance of about 3σ, based on a combination of radio (NVSS) and optical (SDSS) data. (iii) We used aperture photometry on stacked CMB fields at the locations of known large-scale structures, which yielded and confirms a 4σ signal, over a broader spectral range, when using a previously explored catalogue, but shows strong discrepancies in amplitude and scale when compared with expectations. More recent catalogues give more moderate results that range from negligible to 2.5σ at most, but have a more consistent scale and amplitude, the latter being still slightly higher than what is expected from numerical simulations within ΛCMD. Where they can be compared, these measurements are compatible with previous work using data from WMAP, where these scales have been mapped to the limits of cosmic variance. Planck's broader frequency coverage allows for better foreground cleaning and confirms that the signal is achromatic, which makes it preferable for ISW detection. As a final step we used tracers of large-scale structure to filter the CMB data, from which we present maps of the ISW temperature perturbation. These results provide complementary and independent evidence for the existence of a dark energy component that governs the currently accelerated expansion of the Universe.

Original language	English
Article number	A5
Journal	Astronomy and Astrophysics
Volume	571
DOIs	https://doi.org/10.1051/0004-6361/201321526
Publication status	Published - 1 Nov 2014

Keywords

Cosmic background radiation
Dark energy
Galaxies: clusters: general
Large-scale structure of Universe
Methods: data analysis

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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., Bartolo, N., Battaner, E., Benabed, K., Benoît, A., Benoit-Lévy, A., Bernard, J. P., Bersanelli, M., Bielewicz, P., ... Jaffe, A. H. (2014). Planck 2013 results. XIX. The integrated Sachs-Wolfe effect. Astronomy and Astrophysics, 571, [A5]. https://doi.org/10.1051/0004-6361/201321526

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. ; Bartolo, N. ; Battaner, E. ; Benabed, K. ; Benoît, A. ; Benoit-Lévy, A. ; Bernard, J. P. ; Bersanelli, M. ; Bielewicz, P. ; Bobin, J. ; Bock, J. J. ; Bonaldi, A. ; Bonavera, L. ; Bond, J. R. ; Borrill, J. ; Bouchet, F. R. ; Bridges, M. ; Bucher, M. ; Burigana, C. ; Butler, R. C. ; Cardoso, J. F. ; Catalano, A. ; Challinor, A. ; Chamballu, A. ; 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. ; Désert, F. X. ; Dickinson, C. ; Diego, J. M. ; Dolag, K. ; Dole, H. ; Donzelli, S. ; Doré, O. ; Douspis, M. ; Dupac, X. ; Efstathiou, G. ; Enßlin, T. A. ; Eriksen, H. K. ; Fergusson, J. ; Finelli, F. ; Forni, O. ; Fosalba, P. ; Frailis, M. ; Franceschi, E. ; Frommert, M. ; Galeotta, S. ; Ganga, K. ; Génova-Santos, R. T. ; Giard, M. ; Giardino, G. ; Giraud-Héraud, Y. ; González-Nuevo, J. ; Górski, K. M. ; Gratton, S. ; Gregorio, A. ; Gruppuso, A. ; Hansen, F. K. ; Hanson, D. ; Harrison, D. ; Henrot-Versillé, S. ; Hernández-Monteagudo, C. ; Herranz, D. ; Hildebrandt, S. R. ; Hivon, E. ; Ho, S. ; Hobson, M. ; Holmes, W. A. ; Hornstrup, A. ; Hovest, W. ; Huffenberger, K. M. ; Ilić, S. ; Jaffe, A. H. / Planck 2013 results. XIX. The integrated Sachs-Wolfe effect. In: Astronomy and Astrophysics. 2014 ; Vol. 571.

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title = "Planck 2013 results. XIX. The integrated Sachs-Wolfe effect",

abstract = "{\textcopyright} 2014 ESO. Based on cosmic microwave background (CMB) maps from the 2013 Planck Mission data release, this paper presents the detection of the integrated Sachs-Wolfe (ISW) effect, that is, the correlation between the CMB and large-scale evolving gravitational potentials. The significance of detection ranges from 2 to 4σ, depending on which method is used. We investigated three separate approaches, which essentially cover all previous studies, and also break new ground. (i) We correlated the CMB with the Planck reconstructed gravitational lensing potential (for the first time). This detection was made using the lensing-induced bispectrum between the low-{\^a}.,{"} and high-{\^a}.,{"} temperature anisotropies; the correlation between lensing and the ISW effect has a significance close to 2.5σ. (ii) We cross-correlated with tracers of large-scale structure, which yielded a significance of about 3σ, based on a combination of radio (NVSS) and optical (SDSS) data. (iii) We used aperture photometry on stacked CMB fields at the locations of known large-scale structures, which yielded and confirms a 4σ signal, over a broader spectral range, when using a previously explored catalogue, but shows strong discrepancies in amplitude and scale when compared with expectations. More recent catalogues give more moderate results that range from negligible to 2.5σ at most, but have a more consistent scale and amplitude, the latter being still slightly higher than what is expected from numerical simulations within ΛCMD. Where they can be compared, these measurements are compatible with previous work using data from WMAP, where these scales have been mapped to the limits of cosmic variance. Planck's broader frequency coverage allows for better foreground cleaning and confirms that the signal is achromatic, which makes it preferable for ISW detection. As a final step we used tracers of large-scale structure to filter the CMB data, from which we present maps of the ISW temperature perturbation. These results provide complementary and independent evidence for the existence of a dark energy component that governs the currently accelerated expansion of the Universe.",

keywords = "Cosmic background radiation, Dark energy, Galaxies: clusters: general, Large-scale structure of Universe, Methods: data analysis",

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 N. Bartolo and E. Battaner and K. Benabed and A. Beno{\^i}t and A. Benoit-L{\'e}vy and Bernard, {J. P.} and M. Bersanelli and P. Bielewicz and J. Bobin and Bock, {J. J.} and A. Bonaldi and L. Bonavera and Bond, {J. R.} and J. Borrill and Bouchet, {F. R.} 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 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 D{\'e}sert, {F. X.} and C. Dickinson and Diego, {J. M.} and K. Dolag and H. Dole and S. Donzelli and O. Dor{\'e} and M. Douspis and X. Dupac and G. Efstathiou and En{\ss}lin, {T. A.} and Eriksen, {H. K.} and J. Fergusson and F. Finelli and O. Forni and P. Fosalba and M. Frailis and E. Franceschi and M. Frommert and S. Galeotta and K. Ganga and G{\'e}nova-Santos, {R. T.} and M. Giard and G. Giardino and Y. Giraud-H{\'e}raud and J. Gonz{\'a}lez-Nuevo and G{\'o}rski, {K. M.} and S. Gratton and A. Gregorio and A. Gruppuso and Hansen, {F. K.} and D. Hanson and D. Harrison and S. Henrot-Versill{\'e} and C. Hern{\'a}ndez-Monteagudo and D. Herranz and Hildebrandt, {S. R.} and E. Hivon and S. Ho and M. Hobson and Holmes, {W. A.} and A. Hornstrup and W. Hovest and Huffenberger, {K. M.} and S. Ili{\'c} and Jaffe, {A. H.}",

year = "2014",

month = nov,

day = "1",

doi = "10.1051/0004-6361/201321526",

language = "English",

volume = "571",

journal = "Astronomy and Astrophysics",

issn = "0004-6361",

}

Ade, PAR, Aghanim, N, Armitage-Caplan, C, Arnaud, M, Ashdown, M, Atrio-Barandela, F, Aumont, J, Baccigalupi, C, Banday, AJ, Barreiro, RB, Bartlett, JG, Bartolo, N, Battaner, E, Benabed, K, Benoît, A, Benoit-Lévy, A, Bernard, JP, Bersanelli, M, Bielewicz, P, Bobin, J, Bock, JJ, Bonaldi, A, Bonavera, L, Bond, JR, Borrill, J, Bouchet, FR, Bridges, M, Bucher, M, Burigana, C, Butler, RC, Cardoso, JF, Catalano, A, Challinor, A, Chamballu, A, 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, Désert, FX, Dickinson, C, Diego, JM, Dolag, K, Dole, H, Donzelli, S, Doré, O, Douspis, M, Dupac, X, Efstathiou, G, Enßlin, TA, Eriksen, HK, Fergusson, J, Finelli, F, Forni, O, Fosalba, P, Frailis, M, Franceschi, E, Frommert, M, Galeotta, S, Ganga, K, Génova-Santos, RT, Giard, M, Giardino, G, Giraud-Héraud, Y, González-Nuevo, J, Górski, KM, Gratton, S, Gregorio, A, Gruppuso, A, Hansen, FK, Hanson, D, Harrison, D, Henrot-Versillé, S, Hernández-Monteagudo, C, Herranz, D, Hildebrandt, SR, Hivon, E, Ho, S, Hobson, M, Holmes, WA, Hornstrup, A, Hovest, W, Huffenberger, KM, Ilić, S & Jaffe, AH 2014, 'Planck 2013 results. XIX. The integrated Sachs-Wolfe effect', Astronomy and Astrophysics, vol. 571, A5. https://doi.org/10.1051/0004-6361/201321526

Planck 2013 results. XIX. The integrated Sachs-Wolfe effect. / 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.; Bartolo, N.; Battaner, E.; Benabed, K.; Benoît, A.; Benoit-Lévy, A.; Bernard, J. P.; Bersanelli, M.; Bielewicz, P.; Bobin, J.; Bock, J. J.; Bonaldi, A.; Bonavera, L.; Bond, J. R.; Borrill, J.; Bouchet, F. R.; Bridges, M.; Bucher, M.; Burigana, C.; Butler, R. C.; Cardoso, J. F.; Catalano, A.; Challinor, A.; Chamballu, A.; 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.; Désert, F. X.; Dickinson, C.; Diego, J. M.; Dolag, K.; Dole, H.; Donzelli, S.; Doré, O.; Douspis, M.; Dupac, X.; Efstathiou, G.; Enßlin, T. A.; Eriksen, H. K.; Fergusson, J.; Finelli, F.; Forni, O.; Fosalba, P.; Frailis, M.; Franceschi, E.; Frommert, M.; Galeotta, S.; Ganga, K.; Génova-Santos, R. T.; Giard, M.; Giardino, G.; Giraud-Héraud, Y.; González-Nuevo, J.; Górski, K. M.; Gratton, S.; Gregorio, A.; Gruppuso, A.; Hansen, F. K.; Hanson, D.; Harrison, D.; Henrot-Versillé, S.; Hernández-Monteagudo, C.; Herranz, D.; Hildebrandt, S. R.; Hivon, E.; Ho, S.; Hobson, M.; Holmes, W. A.; Hornstrup, A.; Hovest, W.; Huffenberger, K. M.; Ilić, S.; Jaffe, A. H.

In: Astronomy and Astrophysics, Vol. 571, A5, 01.11.2014.

Research output: Contribution to journal › Article › Research › peer-review

TY - JOUR

T1 - Planck 2013 results. XIX. The integrated Sachs-Wolfe effect

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 - Bartolo, N.

AU - Battaner, E.

AU - Benabed, K.

AU - Benoît, A.

AU - Benoit-Lévy, A.

AU - Bernard, J. P.

AU - Bersanelli, M.

AU - Bielewicz, P.

AU - Bobin, J.

AU - Bock, J. J.

AU - Bonaldi, A.

AU - Bonavera, L.

AU - Bond, J. R.

AU - Borrill, J.

AU - Bouchet, F. R.

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 - 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 - Désert, F. X.

AU - Dickinson, C.

AU - Diego, J. M.

AU - Dolag, K.

AU - Dole, H.

AU - Donzelli, S.

AU - Doré, O.

AU - Douspis, M.

AU - Dupac, X.

AU - Efstathiou, G.

AU - Enßlin, T. A.

AU - Eriksen, H. K.

AU - Fergusson, J.

AU - Finelli, F.

AU - Forni, O.

AU - Fosalba, P.

AU - Frailis, M.

AU - Franceschi, E.

AU - Frommert, M.

AU - Galeotta, S.

AU - Ganga, K.

AU - Génova-Santos, R. T.

AU - Giard, M.

AU - Giardino, G.

AU - Giraud-Héraud, Y.

AU - González-Nuevo, J.

AU - Górski, K. M.

AU - Gratton, S.

AU - Gregorio, A.

AU - Gruppuso, A.

AU - Hansen, F. K.

AU - Hanson, D.

AU - Harrison, D.

AU - Henrot-Versillé, S.

AU - Hernández-Monteagudo, C.

AU - Herranz, D.

AU - Hildebrandt, S. R.

AU - Hivon, E.

AU - Ho, S.

AU - Hobson, M.

AU - Holmes, W. A.

AU - Hornstrup, A.

AU - Hovest, W.

AU - Huffenberger, K. M.

AU - Ilić, S.

AU - Jaffe, A. H.

PY - 2014/11/1

Y1 - 2014/11/1

N2 - © 2014 ESO. Based on cosmic microwave background (CMB) maps from the 2013 Planck Mission data release, this paper presents the detection of the integrated Sachs-Wolfe (ISW) effect, that is, the correlation between the CMB and large-scale evolving gravitational potentials. The significance of detection ranges from 2 to 4σ, depending on which method is used. We investigated three separate approaches, which essentially cover all previous studies, and also break new ground. (i) We correlated the CMB with the Planck reconstructed gravitational lensing potential (for the first time). This detection was made using the lensing-induced bispectrum between the low-â.," and high-â.," temperature anisotropies; the correlation between lensing and the ISW effect has a significance close to 2.5σ. (ii) We cross-correlated with tracers of large-scale structure, which yielded a significance of about 3σ, based on a combination of radio (NVSS) and optical (SDSS) data. (iii) We used aperture photometry on stacked CMB fields at the locations of known large-scale structures, which yielded and confirms a 4σ signal, over a broader spectral range, when using a previously explored catalogue, but shows strong discrepancies in amplitude and scale when compared with expectations. More recent catalogues give more moderate results that range from negligible to 2.5σ at most, but have a more consistent scale and amplitude, the latter being still slightly higher than what is expected from numerical simulations within ΛCMD. Where they can be compared, these measurements are compatible with previous work using data from WMAP, where these scales have been mapped to the limits of cosmic variance. Planck's broader frequency coverage allows for better foreground cleaning and confirms that the signal is achromatic, which makes it preferable for ISW detection. As a final step we used tracers of large-scale structure to filter the CMB data, from which we present maps of the ISW temperature perturbation. These results provide complementary and independent evidence for the existence of a dark energy component that governs the currently accelerated expansion of the Universe.

AB - © 2014 ESO. Based on cosmic microwave background (CMB) maps from the 2013 Planck Mission data release, this paper presents the detection of the integrated Sachs-Wolfe (ISW) effect, that is, the correlation between the CMB and large-scale evolving gravitational potentials. The significance of detection ranges from 2 to 4σ, depending on which method is used. We investigated three separate approaches, which essentially cover all previous studies, and also break new ground. (i) We correlated the CMB with the Planck reconstructed gravitational lensing potential (for the first time). This detection was made using the lensing-induced bispectrum between the low-â.," and high-â.," temperature anisotropies; the correlation between lensing and the ISW effect has a significance close to 2.5σ. (ii) We cross-correlated with tracers of large-scale structure, which yielded a significance of about 3σ, based on a combination of radio (NVSS) and optical (SDSS) data. (iii) We used aperture photometry on stacked CMB fields at the locations of known large-scale structures, which yielded and confirms a 4σ signal, over a broader spectral range, when using a previously explored catalogue, but shows strong discrepancies in amplitude and scale when compared with expectations. More recent catalogues give more moderate results that range from negligible to 2.5σ at most, but have a more consistent scale and amplitude, the latter being still slightly higher than what is expected from numerical simulations within ΛCMD. Where they can be compared, these measurements are compatible with previous work using data from WMAP, where these scales have been mapped to the limits of cosmic variance. Planck's broader frequency coverage allows for better foreground cleaning and confirms that the signal is achromatic, which makes it preferable for ISW detection. As a final step we used tracers of large-scale structure to filter the CMB data, from which we present maps of the ISW temperature perturbation. These results provide complementary and independent evidence for the existence of a dark energy component that governs the currently accelerated expansion of the Universe.

KW - Cosmic background radiation

KW - Dark energy

KW - Galaxies: clusters: general

KW - Large-scale structure of Universe

KW - Methods: data analysis

U2 - 10.1051/0004-6361/201321526

DO - 10.1051/0004-6361/201321526

M3 - Article

VL - 571

JO - Astronomy and Astrophysics

JF - Astronomy and Astrophysics

SN - 0004-6361

M1 - A5

ER -