Data di Pubblicazione:
2014
Abstract:
On the arcminute angular scales probed by Planck, the cosmic microwave
background (CMB) anisotropies are gently perturbed by gravitational
lensing. Here we present a detailed study of this effect, detecting
lensing independently in the 100, 143, and 217 GHz frequency bands with
an overall significance of greater than 25sigma. We use
thetemperature-gradient correlations induced by lensing to reconstruct a
(noisy) map of the CMB lensing potential, which provides an integrated
measure of the mass distribution back to the CMB last-scattering
surface. Our lensing potential map is significantly correlated with
other tracers of mass, a fact which we demonstrate using several
representative tracers of large-scale structure. We estimate the power
spectrum of the lensing potential, finding generally good agreement with
expectations from the best-fitting LambdaCDM model for the Planck
temperature power spectrum, showing that this measurement at z = 1100
correctly predicts the properties of the lower-redshift, later-time
structures which source the lensing potential. When combined with the
temperature power spectrum, our measurement provides degeneracy-breaking
power for parameter constraints; it improves CMB-alone constraints on
curvature by a factor of two and also partly breaks the degeneracy
between the amplitude of the primordial perturbation power spectrum and
the optical depth to reionization, allowing a measurement of the optical
depth to reionization which is independent of large-scale polarization
data. Discarding scale information, our measurement corresponds to a 4%
constraint on the amplitude of the lensing potential power spectrum, or
a 2% constraint on the root-mean-squared amplitude of matter
fluctuations at z ~ 2.
background (CMB) anisotropies are gently perturbed by gravitational
lensing. Here we present a detailed study of this effect, detecting
lensing independently in the 100, 143, and 217 GHz frequency bands with
an overall significance of greater than 25sigma. We use
thetemperature-gradient correlations induced by lensing to reconstruct a
(noisy) map of the CMB lensing potential, which provides an integrated
measure of the mass distribution back to the CMB last-scattering
surface. Our lensing potential map is significantly correlated with
other tracers of mass, a fact which we demonstrate using several
representative tracers of large-scale structure. We estimate the power
spectrum of the lensing potential, finding generally good agreement with
expectations from the best-fitting LambdaCDM model for the Planck
temperature power spectrum, showing that this measurement at z = 1100
correctly predicts the properties of the lower-redshift, later-time
structures which source the lensing potential. When combined with the
temperature power spectrum, our measurement provides degeneracy-breaking
power for parameter constraints; it improves CMB-alone constraints on
curvature by a factor of two and also partly breaks the degeneracy
between the amplitude of the primordial perturbation power spectrum and
the optical depth to reionization, allowing a measurement of the optical
depth to reionization which is independent of large-scale polarization
data. Discarding scale information, our measurement corresponds to a 4%
constraint on the amplitude of the lensing potential power spectrum, or
a 2% constraint on the root-mean-squared amplitude of matter
fluctuations at z ~ 2.
Tipologia CRIS:
1.1 Articolo in rivista
Keywords:
gravitational lensing: weak; methods: data analysis; cosmic; background radiation; large-scale structure of Universe
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; S., Basak; 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; T., D�chelette; J., Delabrouille; J., Delouis; F., D�sert; C., Dickinson; J. M., Diego; H., Dole; S., Donzelli; O., Dor�; M., Douspis; J., Dunkley; X., Dupac; G., Efstathiou; T. A., En�lin; H. K., Eriksen; F., Finelli; O., Forni; M., Frailis; E., Franceschi; S., Galeotta; K., Ganga; M., Giard; G., Giardino; Y., Giraud H�raud; J., Gonz�lez Nuevo; K. M., G�rski; S., Gratton; A., Gregorio; A., Gruppuso; J. E., Gudmundsson; 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; A. H., Jaffe; T. R., Jaffe; W. C., Jones; M., Juvela; E., Keih�nen; R., Keskitalo; T. S., Kisner; R., Kneissl; J., Knoche; L., Knox; M., Kunz; H., Kurki Suonio; G., Lagache; A., L�hteenm�ki; J., Lamarre; A., Lasenby; R. J., Laureijs; A., Lavabre; C. R., Lawrence; J. P., Leahy; R., Leonardi; Tavares, J. Le�n.; J., Lesgourgues; A., Lewis; 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; M., Maris; D. J., Marshall; P. G., Martin; E., Mart�nez Gonz�lez; S., Masi; M., Massardi; S., Matarrese; F., Matthai; P., Mazzotta; 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; J. A., Murphy; 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; A. R., Pullen; J. P., Rachen; R., Rebolo; M., Reinecke; M., Remazeilles; C., Renault; 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; D., Scott; M. D., Seiffert; E. P., S.; K., Smith; L. D., Spencer; J., Starck; V., Stolyarov; R., Stompor; R., Sudiwala; R., Sunyaev; F., Sureau; 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; P., Vielva; F., Villa; N., Vittorio; L. A., Wade; B. D., Wandelt; M., White; S. D., M.; D., Yvon; A., Zacchei; A., Zonca
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