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

被引：0

作者：

Ade, P.A.R. ^{[89
]}

Aghanim, N. ^{[62
]}

Armitage-Caplan, C. ^{[95
]}

Arnaud, M. ^{[76
]}

Ashdown, M. ^{[6
,73
]}

Atrio-Barandela, F. ^{[18
]}

Aumont, J. ^{[62
]}

Baccigalupi, C. ^{[88
]}

Banday, A.J. ^{[9
,99
]}

Barreiro, R.B. ^{[70
]}

Bartlett, J.G. ^{[1
,71
]}

Bartolo, N. ^{[34
]}

Battaner, E. ^{[101
]}

Benabed, K. ^{[63
,97
]}

Benoît, A. ^{[60
]}

Benoit-Lévy, A. ^{[25
,63
,97
]}

Bernard, J.-P. ^{[9
,99
]}

Bersanelli, M. ^{[37
,52
]}

Bielewicz, P. ^{[9
,88
,99
]}

Bobin, J. ^{[76
]}

Bock, J.J. ^{[10
,71
]}

Bonaldi, A. ^{[72
]}

Bonavera, L. ^{[70
]}

Bond, J.R. ^{[8
]}

Borrill, J. ^{[13
,92
]}

Bouchet, F.R. ^{[63
,97
]}

Bridges, M. ^{[6
,67
,73
]}

Bucher, M. ^{[1
]}

Burigana, C. ^{[35
,51
]}

Butler, R.C. ^{[51
]}

Cardoso, J.-F. ^{[1
,63
,77
]}

Catalano, A. ^{[75
,78
]}

Challinor, A. ^{[11
,67
,73
]}

Chamballu, A. ^{[15
,62
,76
]}

Chiang, H.C. ^{[7
,29
]}

Chiang, L.-Y. ^{[66
]}

Christensen, P.R. ^{[40
,84
]}

Church, S. ^{[94
]}

Clements, D.L. ^{[58
]}

Colombi, S. ^{[63
,97
]}

Colombo, L.P.L. ^{[24
,71
]}

Couchot, F. ^{[74
]}

Coulais, A. ^{[75
]}

Crill, B.P. ^{[71
,85
]}

Curto, A. ^{[6
,70
]}

Cuttaia, F. ^{[51
]}

Danese, L. ^{[88
]}

Davies, R.D. ^{[72
]}

Davis, R.J. ^{[72
]}

De Bernardis, P. ^{[36
]}

机构：

[1] Ade, P.A.R.

[2] Aghanim, N.

[3] Armitage-Caplan, C.

[4] Arnaud, M.

[5] 6,Ashdown, M.

[6] Atrio-Barandela, F.

[7] Aumont, J.

[8] Baccigalupi, C.

[9] 9,Banday, A.J.

[10] Barreiro, R.B.

[11] 1,Bartlett, J.G.

[12] Bartolo, N.

[13] Battaner, E.

[14] 63,Benabed, K.

[15] Benoît, A.

[16] 25,63,Benoit-Lévy, A.

[17] 9,Bernard, J.-P.

[18] 37,Bersanelli, M.

[19] 9,88,Bielewicz, P.

[20] Bobin, J.

[21] 10,Bock, J.J.

[22] Bonaldi, A.

[23] Bonavera, L.

[24] Bond, J.R.

[25] 13,Borrill, J.

[26] 63,Bouchet, F.R.

[27] 6,67,Bridges, M.

[28] Bucher, M.

[29] 35,Burigana, C.

[30] Butler, R.C.

[31] 1,63,Cardoso, J.-F.

[32] 75,Catalano, A.

[33] 11,67,Challinor, A.

[34] 15,62,Chamballu, A.

[35] 7,Chiang, H.C.

[36] Chiang, L.-Y.

[37] 40,Christensen, P.R.

[38] Church, S.

[39] Clements, D.L.

[40] 63,Colombi, S.

[41] 24,Colombo, L.P.L.

[42] Couchot, F.

[43] Coulais, A.

[44] 71,Crill, B.P.

[45] 6,Curto, A.

[46] Cuttaia, F.

[47] Danese, L.

[48] Davies, R.D.

[49] Davis, R.J.

[50] De Bernardis, P.

来源：

Vielva, P. | 1600年 / EDP Sciences卷 / 571期

关键词：

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. © 2014 ESO;

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Journal article (JA)

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