Data di Pubblicazione:
2014
Abstract:
This paper characterizes the effective beams, the effective beam window
functions and the associated errors for the Planck High Frequency
Instrument (HFI) detectors. The effective beam is theangular response
including the effect of the optics, detectors, data processing and the
scan strategy. The window function is the representation of this beam in
the harmonic domain which is required to recover an unbiased measurement
of the cosmic microwave background angular power spectrum. The HFI is a
scanning instrument and its effective beams are the convolution of: a)
the optical response of the telescope and feeds; b) the processing of
the time-ordered data and deconvolution of the bolometric and electronic
transfer function; and c) the merging of several surveys to produce
maps. The time response transfer functions are measured using
observations of Jupiter and Saturn and by minimizing survey difference
residuals. The scanning beam is the post-deconvolution angular response
of the instrument, and is characterized with observations of Mars. The
main beam solid angles are determined to better than 0.5% at each HFI
frequency band. Observations of Jupiter and Saturn limit near sidelobes
(within 5�) to about 0.1% of the total solid angle. Time response
residuals remain as long tails in the scanning beams, but contribute
less than 0.1% of the total solid angle. The bias and uncertainty in the
beam products are estimated using ensembles of simulated planet
observations that include the impact of instrumental noise and known
systematic effects. The correlation structure of these ensembles is
well-described by five error eigenmodes that are sub-dominant to sample
variance and instrumental noise in the harmonic domain. A suite of
consistency tests provide confidence that the error model represents a
sufficient description of the data. The total error in the effective
beam window functions is below 1% at 100 GHz up to multipole l ~
1500, and below 0.5% at 143 and 217 GHz up to l ~ 2000.
functions and the associated errors for the Planck High Frequency
Instrument (HFI) detectors. The effective beam is theangular response
including the effect of the optics, detectors, data processing and the
scan strategy. The window function is the representation of this beam in
the harmonic domain which is required to recover an unbiased measurement
of the cosmic microwave background angular power spectrum. The HFI is a
scanning instrument and its effective beams are the convolution of: a)
the optical response of the telescope and feeds; b) the processing of
the time-ordered data and deconvolution of the bolometric and electronic
transfer function; and c) the merging of several surveys to produce
maps. The time response transfer functions are measured using
observations of Jupiter and Saturn and by minimizing survey difference
residuals. The scanning beam is the post-deconvolution angular response
of the instrument, and is characterized with observations of Mars. The
main beam solid angles are determined to better than 0.5% at each HFI
frequency band. Observations of Jupiter and Saturn limit near sidelobes
(within 5�) to about 0.1% of the total solid angle. Time response
residuals remain as long tails in the scanning beams, but contribute
less than 0.1% of the total solid angle. The bias and uncertainty in the
beam products are estimated using ensembles of simulated planet
observations that include the impact of instrumental noise and known
systematic effects. The correlation structure of these ensembles is
well-described by five error eigenmodes that are sub-dominant to sample
variance and instrumental noise in the harmonic domain. A suite of
consistency tests provide confidence that the error model represents a
sufficient description of the data. The total error in the effective
beam window functions is below 1% at 100 GHz up to multipole l ~
1500, and below 0.5% at 143 and 217 GHz up to l ~ 2000.
Tipologia CRIS:
1.1 Articolo in rivista
Keywords:
cosmic background radiation; cosmology: observations; instrumentation: detectors; surveys
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; E., Battaner; K., Benabed; A., Beno�t; A., Benoit L�vy; J., Bernard; M., Bersanelli; P., Bielewicz; J., Bobin; J. J., Bock; J. R., Bond; J., Borrill; F. R., Bouchet; J. W., Bowyer; M., Bridges; M., Bucher; C., Burigana; J., Cardoso; A., Catalano; A., Challinor; A., Chamballu; R., Chary; 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; P. d., Bernardis; A. d., Rosa; G. d., Zotti; J., Delabrouille; J., Delouis; F., D�sert; 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; A. A., Fraisse; E., Franceschi; S., Galeotta; K., Ganga; M., Giard; Y., Giraud H�raud; J., Gonz�lez Nuevo; K. M., G�rski; S., Gratton; A., Gregorio; A., Gruppuso; J. E., Gudmundsson; J., Haissinski; F. K., Hansen; D., Hanson; D., Harrison; S., Henrot Versill�; C., Hern�ndez Monteagudo; D., Herranz; S. R., Hildebrandt; E., Hivon; M., Hobson; W. A., Holmes; A., Hornstrup; Z., Hou; 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; J., Lamarre; A., Lasenby; R. J., Laureijs; C. R., Lawrence; R., Leonardi; C., Leroy; J., Lesgourgues; M., Liguori; P. B., Lilje; M., Linden V�rnle; M., L�pez Caniego; P. M., Lubin; J. F., Mac�as P�rez; C. J., Mactavish; B., Maffei; N., Mandolesi; M., Maris; D. J., Marshall; P. G., Martin; E., Mart�nez Gonz�lez; S., Masi; M., Massardi; S., Matarrese; T., Matsumura; F., Matthai; P., Mazzotta; P., Mcgehee; A., Melchiorri; L., Mendes; A., Mennella; M., Migliaccio; S., Mitra; M., Miville Desch�nes; A., Moneti; L., Montier; G., Morgante; D., Mortlock; 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; F., Pasian; G., Patanchon; O., Perdereau; L., Perotto; F., Perrotta; F., Piacentini; M., Piat; E., Pierpaoli; D., Pietrobon; S., Plaszczynski; E., Pointecouteau; A. M., Polegre; G., Polenta; N., Ponthieu; L., Popa; T., Poutanen; G. W., Pratt; G., Pr�zeau; S., Prunet; J., Puget; J. P., Rachen; M., Reinecke; M., Remazeilles; C., Renault; S., Ricciardi; T., Riller; I., Ristorcelli; G., Rocha; C., Rosset; G., Roudier; M., Rowan Robinson; B., Rusholme; M., Sandri; D., Santos; A., Sauv�; G., Savini; D., Scott; E. P., S.; L. D., Spencer; J., Starck; V., Stolyarov; R., Stompor; R., Sudiwala; F., Sureau; D., Sutton; A., Suur Uski; J., Sygnet; J. A., Tauber; D., Tavagnacco; Terenzi, Luca; M., Tomasi; M., Tristram; M., Tucci; G., Umana; L., Valenziano; J., Valiviita; B. V., Tent; P., Vielva; F., Villa; N., Vittorio; L. A., Wade; B. D., Wandelt; D., Yvon; A., Zacchei; A., Zonca
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