Data di Pubblicazione:
2014
Abstract:
The Planck High Frequency Instrument (HFI) spectral response was
determined through a series of ground based tests conducted with the HFI
focal plane in a cryogenic environment prior to launch. The main goal of
the spectral transmission tests was to measure the relative spectral
response (includingthe level of out-of-band signal rejection) of all HFI
detectors to a known source of electromagnetic radiation individually.
This was determined by measuring the interferometric output of a
continuously scanned Fourier transform spectrometer with all HFI
detectors. As there is no on-board spectrometer within HFI, the
ground-based spectral response experiments provide the definitive data
set for the relative spectral calibration of the HFI. Knowledge of the
relative variations in the spectral response between HFI detectors
allows for a more thorough analysis of the HFI data. The spectral
response of the HFI is used in Planck data analysis and component
separation, this includes extraction of CO emission observed within
Planck bands, dust emission, Sunyaev-Zeldovich sources, and intensity to
polarization leakage. The HFI spectral response data have also been used
to provide unit conversion and colour correction analysis tools. While
previous papers describe the pre-flight experiments conducted on the
Planck HFI, this paper focusses on the analysis of the pre-flight
spectral response measurements and the derivation of data products, e.g.
band-average spectra, unit conversion coefficients, and colour
correction coefficients, all with related uncertainties. Verifications
of the HFI spectral response data are provided through comparisons with
photometric HFI flight data. This validation includes use of HFI
zodiacal emission observations to demonstrate out-of-band spectral
signal rejection better than 108. The accuracy of the HFI
relative spectral response data is verified through comparison with
complementary flight-data based unit conversion coefficients and colour
correction coefficients. These coefficients include those based upon HFI
observations of CO, dust, and Sunyaev-Zeldovich emission. General
agreement is observed between the ground-based spectral characterization
of HFI and corresponding in-flight observations, within the quoted
uncertainty of each; explanations are provided for any discrepancies.
determined through a series of ground based tests conducted with the HFI
focal plane in a cryogenic environment prior to launch. The main goal of
the spectral transmission tests was to measure the relative spectral
response (includingthe level of out-of-band signal rejection) of all HFI
detectors to a known source of electromagnetic radiation individually.
This was determined by measuring the interferometric output of a
continuously scanned Fourier transform spectrometer with all HFI
detectors. As there is no on-board spectrometer within HFI, the
ground-based spectral response experiments provide the definitive data
set for the relative spectral calibration of the HFI. Knowledge of the
relative variations in the spectral response between HFI detectors
allows for a more thorough analysis of the HFI data. The spectral
response of the HFI is used in Planck data analysis and component
separation, this includes extraction of CO emission observed within
Planck bands, dust emission, Sunyaev-Zeldovich sources, and intensity to
polarization leakage. The HFI spectral response data have also been used
to provide unit conversion and colour correction analysis tools. While
previous papers describe the pre-flight experiments conducted on the
Planck HFI, this paper focusses on the analysis of the pre-flight
spectral response measurements and the derivation of data products, e.g.
band-average spectra, unit conversion coefficients, and colour
correction coefficients, all with related uncertainties. Verifications
of the HFI spectral response data are provided through comparisons with
photometric HFI flight data. This validation includes use of HFI
zodiacal emission observations to demonstrate out-of-band spectral
signal rejection better than 108. The accuracy of the HFI
relative spectral response data is verified through comparison with
complementary flight-data based unit conversion coefficients and colour
correction coefficients. These coefficients include those based upon HFI
observations of CO, dust, and Sunyaev-Zeldovich emission. General
agreement is observed between the ground-based spectral characterization
of HFI and corresponding in-flight observations, within the quoted
uncertainty of each; explanations are provided for any discrepancies.
Tipologia CRIS:
1.1 Articolo in rivista
Keywords:
instrumentation: detectors; instrumentation: photometers; space vehicles: instruments; cosmology: observations; 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; 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; F., Boulanger; M., Bridges; M., Bucher; C., Burigana; J., Cardoso; 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.; C., Combet; B., Comis; 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; C., Dickinson; J. M., Diego; H., Dole; S., Donzelli; O., Dor�; M., Douspis; X., Dupac; G., Efstathiou; T. A., En�lin; H. K., Eriksen; E., Falgarone; F., Finelli; O., Forni; M., Frailis; 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; 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; W., Hovest; K. M., Huffenberger; G., Hurier; 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; J. P., Leahy; 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; B., Maffei; N., Mandolesi; M., Maris; D. J., Marshall; P. G., Martin; E., Mart�nez Gonz�lez; S., Masi; M., Massardi; S., Matarrese; 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; C., North; 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; 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; B., Rusholme; D., Santos; 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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