Planck 2015 results XXI. The integrated Sachs-Wolfe effect

被引:115
作者
Ade, P. A. R. [101 ]
Aghanim, N. [66 ]
Arnaud, M. [82 ]
Ashdown, M. [8 ,78 ]
Aumont, J. [66 ]
Baccigalupi, C. [98 ]
Banday, A. J. [13 ,113 ]
Barreiro, R. B. [73 ]
Bartolo, N. [35 ,74 ]
Basak, S. [98 ]
Battaner, E. [115 ,116 ]
Benabed, K. [67 ,111 ]
Benoit, A. [64 ]
Benoit-Levy, A. [29 ,67 ,111 ]
Bernard, J. -P. [13 ,113 ]
Bersanelli, M. [38 ,54 ]
Bielewicz, P. [13 ,93 ,98 ]
Bock, J. J. [15 ,75 ]
Bonaldi, A. [76 ]
Bonavera, L. [24 ]
Bond, J. R. [12 ]
Borri, J. [18 ,105 ]
Bouchet, F. R. [67 ,103 ]
Bucher, M. [1 ]
Burigana, C. [36 ,53 ,55 ]
Butler, R. C. [53 ]
Calabrese, E. [108 ]
Cardoso, J. -F. [1 ,67 ,83 ,84 ]
Casaponsa, B. [73 ]
Catalano, A. [81 ,85 ]
Challinor, A. [16 ,70 ,78 ]
Chamballu, A. [20 ,66 ,82 ]
Chiang, H. C. [9 ,32 ]
Christensen, P. R. [41 ,94 ]
Church, S. [107 ]
Clements, D. L. [62 ]
Colombi, S. [67 ,111 ]
Colombo, L. P. L. [28 ,75 ]
Combet, C. [85 ]
Couchot, F. [80 ]
Coulais, A. [81 ]
Crill, B. P. [15 ,38 ]
Curto, A. [8 ,73 ,78 ]
Cuttaia, F. [53 ]
Danese, L. [98 ]
Davies, R. D. [76 ]
Davis, R. J. [76 ]
de Bernardis, P. [37 ]
de Rosa, A. [53 ]
de Zotti, G. [50 ,98 ]
机构
[1] Univ Paris Diderot, APC, CNRS IN2P3, CEA Lrfu,Observ Paris,Sorbonne Paris Cite, 10 Rue Alice Domon & Leonie Duquet, F-75205 Paris 13, France
[2] Aalto Univ, Metsahovi Radio Observ, POB 13000, Aalto 00076, Finland
[3] Aalto Univ, Dept Radio Sci & Engn, POB 13000, Aalto 00076, Finland
[4] African Inst Math Sci, 6-8 Melrose Rd, ZA-7945 Cape Town, South Africa
[5] Agenzia Spaziale Italiana, Sci Data Ctr, Via Politecn Snc, I-00133 Rome, Italy
[6] Aix Marseille Univ, CNRS, LAM, UMR 7326, F-13388 Marseille, France
[7] Aix Marseille Univ, Ctr Phys Theor, 163 Ave Luminy, F-13288 Marseille, France
[8] Univ Cambridge, Cavendish Lab, Astrophys Grp, JJ Thomson Ave, Cambridge CB3 0HE, England
[9] Univ KwaZulu Natal, Sch Math Stat & Comp Sci, Astrophys & Cosmol Res Unit, Westville Campus,Private Bag X54001, ZA-4000 Durban, South Africa
[10] ALMA Santiago Cent Off, Atacama Large Millimeter Submillimeter Array, Alonso Cordova 3107,Casilla 763 0355, Santiago, Chile
[11] CGEE, SCS Qd 9,Lote C,Tone C,4 Andar, BR-70308200 Brasilia, DF, Brazil
[12] Univ Toronto, CITA, 60 St George St, Toronto, ON M5S 3H8, Canada
[13] IRAP, CNRS, 9 Ave Colonel Roche,BP 44346, F-31028 Toulouse 4, France
[14] Trinity Coll Dublin, CRANN, Dublin 2, Ireland
[15] CALTECH, Pasadena, CA 91125 USA
[16] Univ Cambridge, DAMTP, Ctr Theoret Cosmol, Wilberforce Rd, Cambridge CB3 0WA, England
[17] CEFCA, Plaza San Juan,1,Planta 2, 44001 44001, Spain
[18] Lawrence Berkeley Natl Lab, Computat Cosmol Ctr, Berkeley, CA 94720 USA
[19] CSIC, Madrid, Spain
[20] CEA Saclay, DSM Irfu SPP, F-91191 Gif Sur Yvette, France
[21] Tech Univ Denmark, Natl Space Inst, DTU Space, Elektrovej 327, DK-2800 Lyngby, Denmark
[22] Univ Geneva, Dept Phys Theor, 24 Quai E Ansermet, CH-1211 Geneva 4, Switzerland
[23] Univ La Laguna, Dept Astrofis, E-38206 Tenerife, Spain
[24] Univ Oviedo, Dept Fis, Avda Calvo Sotelo S-N, Oviedo 33007, Spain
[25] Univ Toronto, Dept Astron & Astrophys, 50 St George St, Toronto, ON, Canada
[26] Radboud Univ Nijmegen, Dept Astrophys IMAPP, POB 9010, NL-6500 GL Nijmegen, Netherlands
[27] Univ British Columbia, Dept Phys & Astron, 6224 Agr Rd, Vancouver, BC, Canada
[28] Univ Southern Calif, Dana & David Dornsife Coll Letter Arts & Sci, Dept Phys & Astron, Los Angeles, CA 90089 USA
[29] UCL, Dept Phys & Astron, London WC1E 6BT, England
[30] Florida State Univ, Dept Phys, Keen Phys Bldg,77 Chieftan Way, Tallahassee, FL 32306 USA
[31] Univ Helsinki, Dept Phys, Gustaf Hallstromin Katu 2a, Helsinki 00560, Finland
[32] Princeton Univ, Dept Phys, Princeton, NJ 08544 USA
[33] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA
[34] Univ Illinois, Dept Phys, 1110 West Green St, Urbana, IL 61801 USA
[35] Univ Padua, Dipartimento Fis & Astron G Galilei, Via Marzolo 8, I-35131 Padua, Italy
[36] Univ Ferrara, Dipartimento Fis & Sci Terra, Via Saragat 1, I-44122 Ferrara, Italy
[37] Univ Roma La Sapienza, Dipartimento Fis, Ple A Moro 2, I-00133 Rome, Italy
[38] Univ Milan, Dipartimento Fis, Via Celoria 16, I-20133 Milan, Italy
[39] Univ Trieste, Dipartimento Fis, Via A Valerio 2, I-34127 Trieste, Italy
[40] Univ Roma Tor Vergata, Dipartimento Matemat, Via Ric Sci 1, I-00133 Rome, Italy
[41] Niels Bohr Inst, Discovery Ctr, Blegdamsvej 17, DK-1165 Copenhagen, Denmark
[42] Univ Copenhagen, Niels Bohr Inst, Discovery Ctr, Blegdamsvej 17, DK-1165 Copenhagen, Denmark
[43] European So Observ, ESO Vitacura, Alonso Cordova 3107,Casilla 19001, Santiago, Chile
[44] European Space Agcy, ESAC, Planck Sci Off, Madrid 28691, Spain
[45] European Space Agcy, Estec, Keplerlaan 1, NL-2201 AZ Noordwijk, Netherlands
[46] Ist Nazl Fis Nucl, Gran Sasso Sci Inst, Viale F Crispi 7, I-67100 Laquila, Italy
[47] HGSFP, Philosophenweg 16, D-69120 Heidelberg, Germany
[48] Heidelberg Univ, Dept Theoret Phys, Philosophenweg 16, D-69120 Heidelberg, Germany
[49] Aalto Univ, Univ Helsinki, Helsinki Inst Phys, Gustaf Hallstromin Katu 2, Helsinki 00560, Finland
[50] INAF Osservatorio Astron Padova, Vicolo Osservatorio 5, I-35131 Padua, Italy
关键词
cosmology: observations; cosmic background radiation; large-scale structure of Universe; dark energy; galaxies: clusters: general; methods: data analysis; LARGE-SCALE STRUCTURE; PROBE WMAP OBSERVATIONS; DARK ENERGY; CROSS-CORRELATION; SKY SURVEY; REDSHIFT SURVEY; COLD IMPRINT; DATA RELEASE; MICROWAVE; CMB;
D O I
10.1051/0004-6361/201525831
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
This paper presents a study of the integrated Sachs-Wolfe (ISW) effect from the Planck 2015 temperature and polarization data release. This secondary cosmic microwave background (CMB) anisotropy caused by the large-scale time-evolving gravitational potential is probed from different perspectives. The CMB is cross-correlated with different large-scale structure (LSS) tracers: radio sources from the NVSS catalogue; galaxies from the optical SDSS and the infrared WISE surveys; and the Planck 2015 convergence lensing map. The joint cross-correlation of the CMB with the tracers yields a detection at 4 sigma where most of the signal-to-noise is due to the Planck lensing and the NVSS radio catalogue. In fact, the ISW effect is detected from the Planck data only at approximate to 3 sigma (through the ISW-lensing bispectrum), which is similar to the detection level achieved by combining the cross-correlation signal coming from all the galaxy catalogues mentioned above. We study the ability of the ISW effect to place constraints on the dark-energy parameters; in particular, we show that Omega(Lambda) is detected at more than 3 sigma. This cross-correlation analysis is performed only with the Planck temperature data, since the polarization scales available in the 2015 release do not permit significant improvement of the CMB-LSS cross-correlation detectability. Nevertheless, the Planck polarization data are used to study the anomalously large ISW signal previously reported through the aperture photometry on stacked CMB features at the locations of known superclusters and supervoids, which is in conflict with Lambda CDM expectations. We find that the current Planck polarization data do not exclude that this signal could be caused by the ISW effect. In addition, the stacking of the Planck lensing map on the locations of superstructures exhibits a positive cross-correlation with these large-scale structures. Finally, we have improved our previous reconstruction of the ISW temperature fluctuations by combining the information encoded in all the previously mentioned LSS tracers. In particular, we construct a map of the ISW secondary anisotropies and the corresponding uncertainties map, obtained from simulations. We also explore the reconstruction of the ISW anisotropies caused by the large-scale structure traced by the 2MASS Photometric Redshift Survey (2MPZ) by directly inverting the density field into the gravitational potential field.
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页数:30
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ASTRONOMY & ASTROPHYSICS, 2016, 594