Data di Pubblicazione:
2014
Abstract:
Planck has produced detailed all-sky observations over nine frequency
bands between 30 and 857 GHz. These observations allow robust
reconstruction of the primordial cosmic microwave background (CMB)
temperature fluctuations over nearly the full sky, as well as new
constraints on Galactic foregrounds, including thermal dust and line
emission from molecular carbon monoxide (CO). This paper describes the
component separation framework adopted by Planck for many cosmological
analyses, including CMB power spectrum determination and likelihood
construction on large angular scales, studies of primordial
non-Gaussianity and statistical isotropy, the integrated Sachs-Wolfe
effect, gravitational lensing, and searches for topological defects. We
test four foreground-cleaned CMB maps derived using qualitatively
different component separation algorithms. The quality of our
reconstructions is evaluated through detailed simulations and internal
comparisons, and shown through various tests to be internally consistent
and robust for CMB power spectrum and cosmological parameter estimation
up to l = 2000. The parameter constraints on LambdaCDM cosmologies
derived from these maps are consistent with those presented in the
cross-spectrum based Planck likelihood analysis. We choose two of the
CMB maps for specific scientific goals. We also present maps and
frequency spectra of the Galactic low-frequency, CO, and thermal dust
emission. The component maps are found to provide a faithful
representation of the sky, as evaluated by simulations, with the largest
bias seen in the CO component at 3%. For the low-frequency component,
the spectral index varies widely over the sky, ranging from about beta
= -4 to - 2. Considering both morphology and prior knowledge of the low
frequencycomponents, the index map allows us to associate a steep
spectral index (beta< -3.2) with strong anomalous microwave
emission, corresponding to a spinning dust spectrum peaking below 20
GHz, a flat index of beta> -2.3 with strong free-free emission, and
intermediate values with synchrotron emission.
bands between 30 and 857 GHz. These observations allow robust
reconstruction of the primordial cosmic microwave background (CMB)
temperature fluctuations over nearly the full sky, as well as new
constraints on Galactic foregrounds, including thermal dust and line
emission from molecular carbon monoxide (CO). This paper describes the
component separation framework adopted by Planck for many cosmological
analyses, including CMB power spectrum determination and likelihood
construction on large angular scales, studies of primordial
non-Gaussianity and statistical isotropy, the integrated Sachs-Wolfe
effect, gravitational lensing, and searches for topological defects. We
test four foreground-cleaned CMB maps derived using qualitatively
different component separation algorithms. The quality of our
reconstructions is evaluated through detailed simulations and internal
comparisons, and shown through various tests to be internally consistent
and robust for CMB power spectrum and cosmological parameter estimation
up to l = 2000. The parameter constraints on LambdaCDM cosmologies
derived from these maps are consistent with those presented in the
cross-spectrum based Planck likelihood analysis. We choose two of the
CMB maps for specific scientific goals. We also present maps and
frequency spectra of the Galactic low-frequency, CO, and thermal dust
emission. The component maps are found to provide a faithful
representation of the sky, as evaluated by simulations, with the largest
bias seen in the CO component at 3%. For the low-frequency component,
the spectral index varies widely over the sky, ranging from about beta
= -4 to - 2. Considering both morphology and prior knowledge of the low
frequencycomponents, the index map allows us to associate a steep
spectral index (beta< -3.2) with strong anomalous microwave
emission, corresponding to a spinning dust spectrum peaking below 20
GHz, a flat index of beta> -2.3 with strong free-free emission, and
intermediate values with synchrotron emission.
Tipologia CRIS:
1.1 Articolo in rivista
Keywords:
cosmic background radiation
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; 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; F., Boulanger; M., Bridges; M., Bucher; C., Burigana; R. C., Butler; J., Cardoso; G., Castex; A., Catalano; A., Challinor; A., Chamballu; R., Chary; X., Chen; 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; M., Cruz; 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; G., Dobler; H., Dole; S., Donzelli; O., Dor�; M., Douspis; J., Dunkley; X., Dupac; G., Efstathiou; T. A., En�lin; H. K., Eriksen; E., Falgarone; F., Finelli; O., Forni; M., Frailis; A. A., Fraisse; 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; F. K., Hansen; D., Hanson; D. L., Harrison; G., Helou; S., Henrot Versill�; C., Hern�ndez Monteagudo; D., Herranz; S. R., Hildebrandt; E., Hivon; M., Hobson; W. A., Holmes; A., Hornstrup; W., Hovest; G., Huey; K. M., Huffenberger; A. H., Jaffe; T. R., Jaffe; J., Jewell; 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; C. R., Lawrence; M. L., Jeune; S., Leach; 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., 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; K., Mikkelsen; S., Mitra; M., Miville Desch�nes; D., Molinari; 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; I. J., O'Dwyer; S., Osborne; C. A., Oxborrow; F., Paci; L., Pagano; F., Pajot; R., Paladini; D., Paoletti; B., Partridge; F., Pasian; G., Patanchon; T. J., Pearson; O., Perdereau; L., Perotto; F., Perrotta; V., Pettorino; F., Piacentini; M., Piat; E., Pierpaoli; D., Pietrobon; S., Plaszczynski; P., Platania; E., Pointecouteau; G., Polenta; N., Ponthieu; L., Popa; T., Poutanen; G. W., Pratt; G., Pr�zeau; S., Prunet; J., Puget; J. P., Rachen; W. T., Reach; R., Rebolo; M., Reinecke; M., Remazeilles; C., Renault; A., Renzi; S., Ricciardi; T., Riller; I., Ristorcelli; G., Rocha; M., Roman; C., Rosset; G., Roudier; M., Rowan Robinson; Mart�n, J. A. Rubi�o.; B., Rusholme; E., Salerno; M., Sandri; D., Santos; G., Savini; F., Schiavon; D., Scott; M. D., Seiffert; E. P., S.; L. D., Spencer; J., Starck; 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; M., T�rler; 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; I. K., Wehus; A., Wilkinson; J., Xia; D., Yvon; A., Zacchei; A., Zonca
Link alla scheda completa:
Pubblicato in: