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; 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. Maciás-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. Rubinõ-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

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, 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. Maciás-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. Rubinõ-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

Physics

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

48 Scopus citations

Abstract

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 (US)
Article number	A19
Journal	Astronomy and Astrophysics
Volume	571
DOIs	https://doi.org/10.1051/0004-6361/201321526
State	Published - Nov 1 2014

All Science Journal Classification (ASJC) codes

Astronomy and Astrophysics
Space and Planetary Science

Keywords

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

Access to Document

10.1051/0004-6361/201321526

Cite this

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., ... Zonca, A. (2014). Planck 2013 results. XIX. The integrated Sachs-Wolfe effect. Astronomy and Astrophysics, 571, [A19]. https://doi.org/10.1051/0004-6361/201321526

@article{9658bb32c69c4c45937855d6d5eba5fa,

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

abstract = "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.} and Jaffe, {T. R.} and J. Jasche and Jones, {W. C.} and M. Juvela and E. Keih{\"a}nen and R. Keskitalo and Kisner, {T. S.} and J. Knoche and L. Knox and M. Kunz and H. Kurki-Suonio and G. Lagache and A. L{\"a}hteenm{\"a}ki and Lamarre, {J. M.} and M. Langer and A. Lasenby and Laureijs, {R. J.} and Lawrence, {C. R.} and Leahy, {J. P.} and R. Leonardi and J. Lesgourgues and M. Liguori and Lilje, {P. B.} and M. Linden-V{\o}rnle and M. L{\'o}pez-Caniego and Lubin, {P. M.} and Maci{\'a}s-P{\'e}rez, {J. F.} and B. Maffei and D. Maino and N. Mandolesi and A. Mangilli and A. Marcos-Caballero and M. Maris and Marshall, {D. J.} and Martin, {P. G.} and E. Mart{\'i}nez-Gonz{\'a}lez and S. Masi and M. Massardi and S. Matarrese and F. Matthai and P. Mazzotta and Meinhold, {P. R.} and A. Melchiorri and L. Mendes and A. Mennella and M. Migliaccio and S. Mitra and Miville-Desch{\^e}nes, {M. A.} and A. Moneti and L. Montier and G. Morgante and D. Mortlock and A. Moss and D. Munshi and P. Naselsky and F. Nati and P. Natoli and Netterfield, {C. B.} and N{\o}rgaard-Nielsen, {H. U.} and F. Noviello and D. Novikov and I. Novikov and S. Osborne and Oxborrow, {C. A.} and F. Paci and L. Pagano and F. Pajot 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. Pr{\'e}zeau and S. Prunet and Puget, {J. L.} and Rachen, {J. P.} and B. Racine and R. Rebolo and M. Reinecke and M. Remazeilles and C. Renault and A. Renzi and S. Ricciardi and T. Riller and I. Ristorcelli and G. Rocha and C. Rosset and G. Roudier and M. Rowan-Robinson and Rubin{\~o}-Mart{\'i}n, {J. A.} and B. Rusholme and M. Sandri and D. Santos and G. Savini and Schaefer, {B. M.} and F. Schiavon and D. Scott and Seiffert, {M. D.} 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 P. Sutter 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 G. Umana and L. Valenziano and J. Valiviita and {Van Tent}, B. and J. Varis and M. Viel and P. Vielva and F. Villa and N. Vittorio and Wade, {L. A.} and Wandelt, {B. D.} and M. White and Xia, {J. Q.} and D. Yvon and A. Zacchei and A. Zonca",

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year = "2014",

month = nov,

day = "1",

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

language = "English (US)",

volume = "571",

journal = "Astronomy and Astrophysics",

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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, Jaffe, TR, Jasche, J, Jones, WC, Juvela, M, Keihänen, E, Keskitalo, R, Kisner, TS, Knoche, J, Knox, L, Kunz, M, Kurki-Suonio, H, Lagache, G, Lähteenmäki, A, Lamarre, JM, Langer, M, Lasenby, A, Laureijs, RJ, Lawrence, CR, Leahy, JP, Leonardi, R, Lesgourgues, J, Liguori, M, Lilje, PB, Linden-Vørnle, M, López-Caniego, M, Lubin, PM, Maciás-Pérez, JF, Maffei, B, Maino, D, Mandolesi, N, Mangilli, A, Marcos-Caballero, A, Maris, M, Marshall, DJ, Martin, PG, Martínez-González, E, Masi, S, Massardi, M, Matarrese, S, Matthai, F, Mazzotta, P, Meinhold, PR, Melchiorri, A, Mendes, L, Mennella, A, Migliaccio, M, Mitra, S, Miville-Deschênes, MA, Moneti, A, Montier, L, Morgante, G, Mortlock, D, Moss, A, Munshi, D, 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, 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, Prézeau, G, Prunet, S, Puget, JL, Rachen, JP, Racine, B, Rebolo, R, Reinecke, M, Remazeilles, M, Renault, C, Renzi, A, Ricciardi, S, Riller, T, Ristorcelli, I, Rocha, G, Rosset, C, Roudier, G, Rowan-Robinson, M, Rubinõ-Martín, JA, Rusholme, B, Sandri, M, Santos, D, Savini, G, Schaefer, BM, Schiavon, F, Scott, D, Seiffert, MD, Shellard, EPS, Spencer, LD, Starck, JL, Stolyarov, V, Stompor, R, Sudiwala, R, Sunyaev, R, Sureau, F, Sutter, P, Sutton, D, Suur-Uski, AS, Sygnet, JF, Tauber, JA, Tavagnacco, D, Terenzi, L, Toffolatti, L, Tomasi, M, Tristram, M, Tucci, M, Tuovinen, J, Umana, G, Valenziano, L, Valiviita, J, Van Tent, B, Varis, J, Viel, M, Vielva, P, Villa, F, Vittorio, N, Wade, LA, Wandelt, BD, White, M, Xia, JQ, Yvon, D, Zacchei, A & Zonca, A 2014, 'Planck 2013 results. XIX. The integrated Sachs-Wolfe effect', Astronomy and Astrophysics, vol. 571, A19. https://doi.org/10.1051/0004-6361/201321526

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.

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PY - 2014/11/1

Y1 - 2014/11/1

N2 - 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 - 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

UR - http://www.scopus.com/inward/record.url?scp=84949121404&partnerID=8YFLogxK

UR - http://www.scopus.com/inward/citedby.url?scp=84949121404&partnerID=8YFLogxK

U2 - 10.1051/0004-6361/201321526

DO - 10.1051/0004-6361/201321526

M3 - Article

AN - SCOPUS:84949121404

VL - 571

JO - Astronomy and Astrophysics

JF - Astronomy and Astrophysics

SN - 0004-6361

M1 - A19

ER -

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

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