Sökning: WFRF:(Catalano A.) > XXI. The integrated...
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000 | 12074naa a2203145 4500 | |
001 | oai:DiVA.org:su-140354 | |
003 | SwePub | |
008 | 170308s2016 | |||||||||||000 ||eng| | |
024 | 7 | a https://urn.kb.se/resolve?urn=urn:nbn:se:su:diva-1403542 URI |
024 | 7 | a https://doi.org/10.1051/0004-6361/2015258312 DOI |
040 | a (SwePub)su | |
041 | a engb eng | |
042 | 9 SwePub | |
072 | 7 | a ref2 swepub-contenttype |
072 | 7 | a art2 swepub-publicationtype |
100 | 1 | a Ade, P. A. R.4 aut |
245 | 1 0 | a XXI. The integrated Sachs-Wolfe effect |
264 | c 2016-09-20 | |
264 | 1 | b EDP Sciences,c 2016 |
338 | a print2 rdacarrier | |
520 | a 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. | |
650 | 7 | a NATURVETENSKAPx Fysikx Astronomi, astrofysik och kosmologi0 (SwePub)103052 hsv//swe |
650 | 7 | a NATURAL SCIENCESx Physical Sciencesx Astronomy, Astrophysics and Cosmology0 (SwePub)103052 hsv//eng |
653 | a cosmology: observations | |
653 | a cosmic background radiation | |
653 | a large-scale structure of Universe | |
653 | a dark energy | |
653 | a galaxies: clusters: general | |
653 | a methods: data analysis | |
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710 | 2 | a Stockholms universitetb Fysikum4 org |
773 | 0 | t Astronomy and Astrophysicsd : EDP Sciencesg 594q 594x 0004-6361x 1432-0746 |
856 | 4 | u https://doi.org/10.1051/0004-6361/201525831y Fulltext |
856 | 4 | u https://www.aanda.org/articles/aa/pdf/2016/10/aa25831-15.pdf |
856 | 4 8 | u https://urn.kb.se/resolve?urn=urn:nbn:se:su:diva-140354 |
856 | 4 8 | u https://doi.org/10.1051/0004-6361/201525831 |
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