Data di Pubblicazione:
2014
Abstract:
The European Space Agency's Planck satellite, dedicated to studying the
early Universe and its subsequent evolution, was launched 14 May 2009
and has been scanning the microwave and submillimetre sky continuously
since 12 August 2009. In March 2013, ESA and the Planck Collaboration
released the initial cosmology products based on the first 15.5 months
of Planck data, along with a set of scientific and technical papers and
a web-based explanatory supplement. This paper gives an overview of the
mission and its performance, the processing, analysis, and
characteristics of the data, the scientific results, and the science
data products and papers in the release. The science products include
maps of the cosmic microwave background (CMB) and diffuse extragalactic
foregrounds, a catalogue of compact Galactic and extragalactic sources,
and a list of sources detected through the Sunyaev-Zeldovich effect. The
likelihood code used to assess cosmological models against the Planck
data and a lensing likelihood are described. Scientific results include
robust support for the standard six-parameter LambdaCDM model of
cosmology and improved measurements of its parameters, including a
highly significant deviation from scale invariance of the primordial
power spectrum. The Planck values for these parameters and others
derived from them are significantly different from those previously
determined. Several large-scale anomalies in the temperature
distribution of the CMB, first detected by WMAP, are confirmed with
higher confidence. Planck sets new limits on the number and mass of
neutrinos, and has measured gravitational lensing of CMB anisotropies at
greater than 25sigma. Planck finds no evidence for non-Gaussianity in
the CMB. Planck's results agree well with results from the measurements
of baryon acoustic oscillations. Planck finds a lower Hubble constant
than found in some more local measures. Some tension is also present
between the amplitude of matter fluctuations (sigma8)
derived from CMB data and that derived from Sunyaev-Zeldovich data. The
Planck and WMAP power spectra are offset from each other by an average
level of about 2% around the first acoustic peak. Analysis of Planck
polarization data is not yet mature, therefore polarization results are
not released, although the robust detection of E-mode polarization
around CMB hot and cold spots is shown graphically.
early Universe and its subsequent evolution, was launched 14 May 2009
and has been scanning the microwave and submillimetre sky continuously
since 12 August 2009. In March 2013, ESA and the Planck Collaboration
released the initial cosmology products based on the first 15.5 months
of Planck data, along with a set of scientific and technical papers and
a web-based explanatory supplement. This paper gives an overview of the
mission and its performance, the processing, analysis, and
characteristics of the data, the scientific results, and the science
data products and papers in the release. The science products include
maps of the cosmic microwave background (CMB) and diffuse extragalactic
foregrounds, a catalogue of compact Galactic and extragalactic sources,
and a list of sources detected through the Sunyaev-Zeldovich effect. The
likelihood code used to assess cosmological models against the Planck
data and a lensing likelihood are described. Scientific results include
robust support for the standard six-parameter LambdaCDM model of
cosmology and improved measurements of its parameters, including a
highly significant deviation from scale invariance of the primordial
power spectrum. The Planck values for these parameters and others
derived from them are significantly different from those previously
determined. Several large-scale anomalies in the temperature
distribution of the CMB, first detected by WMAP, are confirmed with
higher confidence. Planck sets new limits on the number and mass of
neutrinos, and has measured gravitational lensing of CMB anisotropies at
greater than 25sigma. Planck finds no evidence for non-Gaussianity in
the CMB. Planck's results agree well with results from the measurements
of baryon acoustic oscillations. Planck finds a lower Hubble constant
than found in some more local measures. Some tension is also present
between the amplitude of matter fluctuations (sigma8)
derived from CMB data and that derived from Sunyaev-Zeldovich data. The
Planck and WMAP power spectra are offset from each other by an average
level of about 2% around the first acoustic peak. Analysis of Planck
polarization data is not yet mature, therefore polarization results are
not released, although the robust detection of E-mode polarization
around CMB hot and cold spots is shown graphically.
Tipologia CRIS:
1.1 Articolo in rivista
Keywords:
cosmology: observations; cosmic background radiation; space vehicles: instruments; instrumentation: detectors
Elenco autori:
P., Collaboration; P. A., R.; N., Aghanim; M. I., R.; C., Armitage Caplan; M., Arnaud; M., Ashdown; F., Atrio Barandela; J., Aumont; H., Aussel; C., Baccigalupi; A. J., Banday; R. B., Barreiro; R., Barrena; M., Bartelmann; J. G., Bartlett; N., Bartolo; S., Basak; E., Battaner; R., Battye; K., Benabed; A., Beno�t; A., Benoit L�vy; J., Bernard; M., Bersanelli; B., Bertincourt; M., Bethermin; P., Bielewicz; I., Bikmaev; A., Blanchard; J., Bobin; J. J., Bock; H., B�hringer; A., Bonaldi; L., Bonavera; J. R., Bond; J., Borrill; F. R., Bouchet; F., Boulanger; H., Bourdin; J. W., Bowyer; M., Bridges; M. L., Brown; M., Bucher; R., Burenin; C., Burigana; R. C., Butler; E., Calabrese; B., Cappellini; J., Cardoso; R., Carr; P., Carvalho; M., Casale; G., Castex; A., Catalano; A., Challinor; A., Chamballu; R., Chary; X., Chen; H. C., Chiang; L., Chiang; G., Chon; P. R., Christensen; E., Churazov; S., Church; M., Clemens; D. L., Clements; S., Colombi; L. P., L.; C., Combet; B., Comis; F., Couchot; A., Coulais; B. P., Crill; M., Cruz; A., Curto; F., Cuttaia; A. D., Silva; H., Dahle; L., Danese; R. D., Davies; R. J., Davis; P. d., Bernardis; A. d., Rosa; G. d., Zotti; T., D�chelette; J., Delabrouille; J., Delouis; J., D�mocl�s; F., D�sert; J., Dick; C., Dickinson; J. M., Diego; K., Dolag; H., Dole; S., Donzelli; O., Dor�; M., Douspis; A., Ducout; J., Dunkley; X., Dupac; G., Efstathiou; F., Elsner; T. A., En�lin; H. K., Eriksen; O., Fabre; E., Falgarone; M. C., Falvella; Y., Fantaye; J., Fergusson; C., Filliard; F., Finelli; I., Flores Cacho; S., Foley; O., Forni; P., Fosalba; M., Frailis; A. A., Fraisse; E., Franceschi; M., Freschi; S., Fromenteau; M., Frommert; T. C., Gaier; S., Galeotta; J., Gallegos; S., Galli; B., Gandolfo; K., Ganga; C., Gauthier; R. T., G�nova Santos; T., Ghosh; M., Giard; G., Giardino; M., Gilfanov; D., Girard; Y., Giraud H�raud; E., Gjerl�w; J., Gonz�lez Nuevo; K. M., G�rski; S., Gratton; A., Gregorio; A., Gruppuso; J. E., Gudmundsson; J., Haissinski; J., Hamann; F. K., Hansen; M., Hansen; D., Hanson; D. L., Harrison; A., Heavens; G., Helou; A., Hempel; S., Henrot Versill�; C., Hern�ndez Monteagudo; D., Herranz; S. R., Hildebrandt; E., Hivon; S., Ho; M., Hobson; W. A., Holmes; A., Hornstrup; Z., Hou; W., Hovest; G., Huey; K. M., Huffenberger; G., Hurier; S., Ilic; A. H., Jaffe; T. R., Jaffe; J., Jasche; J., Jewell; W. C., Jones; M., Juvela; P., Kalberla; P., Kangaslahti; E., Keih�nen; J., Kerp; R., Keskitalo; I., Khamitov; K., Kiiveri; J., Kim; T. S., Kisner; R., Kneissl; J., Knoche; L., Knox; M., Kunz; H., Kurki Suonio; F., Lacasa; G., Lagache; A., L�hteenm�ki; J., Lamarre; M., Langer; A., Lasenby; M., Lattanzi; R. J., Laureijs; A., Lavabre; C. R., Lawrence; M. L., Jeune; S., Leach; J. P., Leahy; R., Leonardi; Tavares, J. Le�n.; C., Leroy; J., Lesgourgues; A., Lewis; C., Li; A., Liddle; M., Liguori; P. B., Lilje; M., Linden V�rnle; V., Lindholm; M., L�pez Caniego; S., Lowe; P. M., Lubin; J. F., Mac�as P�rez; C. J., Mactavish; B., Maffei; G., Maggio; D., Maino; N., Mandolesi; A., Mangilli; A., Marcos Caballero; D., Marinucci; M., Maris; F., Marleau; D. J., Marshall; P. G., Martin; E., Mart�nez Gonz�lez; S., Masi; M., Massardi; S., Matarrese; T., Matsumura; F., Matthai; L., Maurin; P., Mazzotta; A., Mcdonald; J. D., Mcewen; P., Mcgehee; S., Mei; P. R., Meinhold; A., Melchiorri; J., Melin; L., Mendes; E., Menegoni; A., Mennella; M., Migliaccio; K., Mikkelsen; M., Millea; R., Miniscalco; S., Mitra; M., Miville Desch�nes; D., Molinari; A., Moneti; L., Montier; G., Morgante; N., Morisset; D., Mortlock; A., Moss; D., Munshi; J. A., Murphy; P., Naselsky; F., Nati; P., Natoli; M., Negrello; N. P., H.; C. B., Netterfield; H. U., N�rgaard Nielsen; C., North; F., Noviello; D., Novikov; I., Novikov; I. J., O'Dwyer; F., Orieux; S., Osborne; C., O'Sullivan; C. A., Oxborrow; F., Paci; L., Pagano; F., Pajot; R., Paladini; S., Pandolfi;
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