Data di Pubblicazione:
2014
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 4sigma, 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 2.5sigma. (ii) We cross-correlated
with tracers of large-scale structure, which yielded a significance of
about 3sigma, 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 4sigma 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
2.5sigma at most, but have a more consistent scale and amplitude, the
latter being still slightly higher than what is expected from numerical
simulations within LambdaCMD. 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.
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 4sigma, 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 2.5sigma. (ii) We cross-correlated
with tracers of large-scale structure, which yielded a significance of
about 3sigma, 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 4sigma 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
2.5sigma at most, but have a more consistent scale and amplitude, the
latter being still slightly higher than what is expected from numerical
simulations within LambdaCMD. 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.
Tipologia CRIS:
1.1 Articolo in rivista
Keywords:
cosmic background radiation; large-scale structure of Universe; dark energy; galaxies: clusters: general; methods: data analysis
Elenco autori:
P., Collaboration; P. A., R.; 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., Beno�t; A., Benoit L�vy; J., 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., Cardoso; A., Catalano; A., Challinor; A., Chamballu; H. C., Chiang; L., Chiang; P. R., Christensen; S., Church; D. L., Clements; S., Colombi; L. P., L.; F., Couchot; A., Coulais; B. P., Crill; A., Curto; F., Cuttaia; L., Danese; R. D., Davies; R. J., Davis; P. d., Bernardis; A. d., Rosa; G. d., Zotti; J., Delabrouille; J., Delouis; F., D�sert; C., Dickinson; J. M., Diego; K., Dolag; H., Dole; S., Donzelli; O., Dor�; M., Douspis; X., Dupac; G., Efstathiou; T. A., En�lin; H. K., Eriksen; J., Fergusson; F., Finelli; O., Forni; P., Fosalba; M., Frailis; E., Franceschi; M., Frommert; S., Galeotta; K., Ganga; R. T., G�nova Santos; M., Giard; G., Giardino; Y., Giraud H�raud; J., Gonz�lez Nuevo; K. M., G�rski; S., Gratton; A., Gregorio; A., Gruppuso; F. K., Hansen; D., Hanson; D., Harrison; S., Henrot Versill�; C., Hern�ndez Monteagudo; D., Herranz; S. R., Hildebrandt; E., Hivon; S., Ho; M., Hobson; W. A., Holmes; A., Hornstrup; W., Hovest; K. M., Huffenberger; S., Ilic; A. H., Jaffe; T. R., Jaffe; J., Jasche; W. C., Jones; M., Juvela; E., Keih�nen; R., Keskitalo; T. S., Kisner; J., Knoche; L., Knox; M., Kunz; H., Kurki Suonio; G., Lagache; A., L�hteenm�ki; J., 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 V�rnle; M., L�pez Caniego; P. M., Lubin; J. F., Mac�as P�rez; B., Maffei; D., Maino; N., Mandolesi; A., Mangilli; A., Marcos Caballero; M., Maris; D. J., Marshall; P. G., Martin; E., Mart�nez Gonz�lez; S., Masi; M., Massardi; S., Matarrese; F., Matthai; P., Mazzotta; P. R., Meinhold; A., Melchiorri; L., Mendes; A., Mennella; M., Migliaccio; S., Mitra; M., Miville Desch�nes; A., Moneti; L., Montier; G., Morgante; D., Mortlock; A., Moss; D., Munshi; P., Naselsky; F., Nati; P., Natoli; C. B., Netterfield; H. U., N�rgaard 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., Pr�zeau; S., Prunet; J., 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; Mart�n, J. A. Rubi�o.; B., Rusholme; M., Sandri; D., Santos; G., Savini; B. M., Schaefer; F., Schiavon; D., Scott; M. D., Seiffert; E. P., S.; L. D., Spencer; J., Starck; V., Stolyarov; R., Stompor; R., Sudiwala; R., Sunyaev; F., Sureau; P., Sutter; D., Sutton; A., Suur Uski; J., Sygnet; J. A., Tauber; D., Tavagnacco; Terenzi, Luca; L., Toffolatti; M., Tomasi; M., Tristram; M., Tucci; J., Tuovinen; G., Umana; L., Valenziano; J., Valiviita; B. V., Tent; J., Varis; M., Viel; P., Vielva; F., Villa; N., Vittorio; L. A., Wade; B. D., Wandelt; M., White; J., Xia; D., Yvon; A., Zacchei; A., Zonca
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