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

被引：159

作者：

Ade, P. A. R. ^{[88
]}

Aghanim, N.

Armitage-Caplan, C. ^{[94
]}

Arnaud, M. ^{[75
]}

Ashdown, M. ^{[72
]}

Atrio-Barandelals, E. ^{[6
]}

Aumont, J. ^{[18
]}

Baccigalupi, C.

Banday, A. J.

Barreiro, R. B. ^{[9
,98
]}

Bartlett, J. G. ^{[69
]}

Bartolo, N. ^{[34
]}

Battaner, E. ^{[100
]}

Benabed, K. ^{[61
,62
,96
]}

Benoit, A. ^{[59
]}

Benoit-Levy, A. ^{[25
,61
,62
,96
]}

Bernard, J. -P. ^{[9
,98
]}

Bersanelli, M. ^{[37
,51
]}

Bielewicz, P. ^{[9
,98
]}

Bobin, J. ^{[75
]}

Bock, J. J. ^{[10
,70
]}

Bonaldi, A. ^{[71
]}

Bonavera, L. ^{[69
]}

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

Borrill, J. ^{[13
,91
]}

Bouchet, F. R. ^{[61
,62
,96
]}

Bridges, M. ^{[6
,66
,72
]}

Bucher, M. ^{[1
]}

Burigana, C. ^{[35
,50
]}

Butler, R. C. ^{[50
]}

Cardoso, J. -F. ^{[1
,61
,62
,76
,77
]}

Catalano, A. ^{[74
,78
]}

Challinor, A. ^{[10
,11
,66
,72
]}

Chamballu, A. ^{[15
,75
]}

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

Chiang, L. -Y. ^{[65
]}

Christensen, P. R. ^{[39
,84
]}

Church, S. ^{[93
]}

Clements, D. L. ^{[57
]}

Colombi, S. ^{[61
,62
,96
]}

Colombo, L. P. L. ^{[24
,70
]}

Couchot, E. ^{[73
]}

Coulais, A. ^{[74
]}

Crill, B. P. ^{[70
,85
]}

Curto, A. ^{[6
,69
]}

Cuttaia, E. ^{[50
]}

Danese, L.

Davies, R. D. ^{[71
]}

Davis, R. J. ^{[71
]}

de Bernardis, P. ^{[36
]}

机构：

[1] Univ Paris Diderot, CNRS, IN2P3, CEA Irfu,Observ Paris,Sorbonne Paris Cite,APC, F-75205 Paris 13, France

[2] Aalto Univ Metsahovi Radio Observ, Kylmala 02540, Finland

[3] African Inst Math Sci, ZA-7945 Cape Town, South Africa

[4] Agenzia Spaziale Italiana, Sci Data Ctr, I-00133 Rome, Italy

[5] Agenzia Spaziale Italiana, I-00198 Rome, Italy

[6] Univ Cambridge, Cavendish Lab, Astrophys Grp, Cambridge CB3 0HE, England

[7] Univ KwaZulu Natal, Sch Math Stat & Comp Sci, Astrophys & Cosmol Res Unit, ZA-4000 Durban, South Africa

[8] Univ Toronto, CITA, Toronto, ON M5S 3H8, Canada

[9] CNRS, IRAP, F-31028 Toulouse 4, France

[10] CALTECH, Pasadena, CA USA

[11] Univ Cambridge, Ctr Theoret Technol, DAMTP, Cambridge CB3 0WA, England

[12] CEFCA, Teruel 44001, Spain

[13] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Computat Cosmol Ctr, Berkeley, CA 94720 USA

[14] CSIC, E-28006 Madrid, Spain

[15] CEA Saclay, DSM Irfu SPP, F-91191 Gif Sur Yvette, France

[16] Tech Univ Denmark, Natl Space Inst, DTU Space, DK-2800 Lyngby, Denmark

[17] Univ Geneva, Dept Phys Theor, CH-1211 Geneva 4, Switzerland

[18] Univ Salamanca, Fac Ciencias, Dept Fis Fundamental, E-37008 Salamanca, Spain

[19] Univ Oviedo, Dept Fis, Oviedo 33007, Spain

[20] Univ Toronto, Dept Astron & Astrophys, Toronto, ON, Canada

[21] Radboud Univ Nijmegen, IMAPP, Dept Astrophys, NL-6500 GL Nijmegen, Netherlands

[22] Univ Calif Berkeley, Dept Elect Engn & Comp Sci, Berkeley, CA 94720 USA

[23] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V5Z 1M9, Canada

[24] Univ So Calif, Dana & David Dornife Coll Letter Arts & Sci, Dept Phys & Astron, Los Angeles, CA 90089 USA

[25] UCL, Dept Phys & Astron, London WC1E 6BT, England

[26] Carnegie Mellon Univ, Dept Phys, Pittsburgh, PA 15213 USA

[27] Florida State Univ, Dept Phys, Pittsburgh, PA 15213 USA

[28] Univ Helsinki, Dept Phys, FIN-00014 Helsinki, Finland

[29] Princeton Univ, Dept Phys, Princeton, NJ 08544 USA

[30] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA

[31] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA

[32] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA

[33] Univ Illinois, Dept Phys, Urbana, IL USA

[34] Univ Padua, Dipartimento Fis & Astron G Galilei, I-35131 Padua, Italy

[35] Univ Ferrara, Dipartimento Fis & Sci Terra, I-44122 Ferrara, Italy

[36] Univ Roma La Sapienza, Dipartimento Fis, I-00185 Rome, Italy

[37] Univ Milan, Dipartimento Fis, I-20133 Milan, Italy

[38] Univ Trieste, Dipartmento Fis, I-34127 Trieste, Italy

[39] Niels Bohr Inst, Discovery Ctr, DK-2100 Copenhagen, Denmark

[40] Univ La Laguna, Dpto Astrofis, E-38206 Tenerife, Spain

[41] European Space Agcy, ESAC, Planck Sci Off, Madrid 28692, Spain

[42] European Space Agcy, Estec, NL-2201 AZ Noordwijk, Netherlands

[43] Haverford Coll, Dept Astrophys, Haverford, PA 19041 USA

[44] Aalto Univ, Univ Helsinki, Helsinki Inst Phys, FIN-00014 Helsinki, Finland

[45] Osserv Astrofis Catania, INAF, I-95123 Catania, Italy

[46] Osserv Astron Padova, INAF, Padua, Italy

[47] Osserv Astron Roma, INAF, I-00040 Monte Porzio Catone, Italy

[48] Osserv Astron Trieste, INAF, I-34143 Trieste, Italy

[49] Ist Radioastron, INAF, I-40129 Bologna, Italy

[50] IASF Bologna, INAF, I-40129 Bologna, Italy

来源：

ASTRONOMY & ASTROPHYSICS | 2014年 / 571卷

关键词：

cosmic background radiation; large-scale structure of Universe; dark energy; galaxies: clusters: general; methods: data analysis; PROBE WMAP OBSERVATIONS; CROSS-CORRELATION; DARK ENERGY; POWER SPECTRA; NON-GAUSSIANITY; RADIO GALAXIES; DATA RELEASE; MICROWAVE; SKY; NVSS;

D O I：

10.1051/0004-6361/201321526

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

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 4 sigma, 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-l and high-l temperature anisotropies; the correlation between lensing and the ISW effect has a significance close to 2.5 sigma. (ii) We cross-correlated with tracers of large-scale structure, which yielded a significance of about 3 sigma, 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 4 sigma 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 2.5 sigma at most, but have a more consistent scale and amplitude, the latter being still slightly higher than what is expected from numerical simulations within Lambda CMD. 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.

引用

页数：23

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