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Planck pre-launch status: High Frequency Instrument polarization calibration

Rosset, C., Tristram, M., Ponthieu, N., Ade, Peter A. R., Aumont, J., Catalano, A., Conversi, L., Couchot, F., Crill, B. P., Désert, F. X., Ganga, K., Giard, M., Giraud-Héraud, Y., Haïssinski, J., Henrot-Versillé, S., Holmes, W., Jones, W. C., Lamarre, J. M., Lange, A., Leroy, C., Macías-Pérez, J., Maffei, B., de Marcillac, P., Miville-Deschênes, M. A., Montier, L., Noviello, F., Pajot, F., Perdereau, O., Piacentini, F., Piat, M., Plaszczynski, S., Pointecouteau, E., Puget, J. L., Ristorcelli, I., Savini, G., Sudiwala, Rashmikant, Veneziani, M. and Yvon, D. 2010. Planck pre-launch status: High Frequency Instrument polarization calibration. Astronomy and Astrophysics 520 , A13. 10.1051/0004-6361/200913054

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Abstract

The High Frequency Instrument of Planck will map the entire sky in the millimeter and sub-millimeter domain from 100 to 857 GHz with unprecedented sensitivity to polarization (ΔP/Tcmb ~ 4 × 10(-6) for P either Q or U and Tcmb 2.7 K) at 100, 143, 217 and 353 GHz. It will lead to major improvements in our understanding of the cosmic microwave background anisotropies and polarized foreground signals. Planck will make high resolution measurements of the E-mode spectrum (up to ~ 1500) and will also play a prominent role in the search for the faint imprint of primordial gravitational waves on the CMB polarization. This paper addresses the effects of calibration of both temperature (gain) and polarization (polarization efficiency and detector orientation) on polarization measurements. The specific requirements on the polarization parameters of the instrument are set and we report on their pre-flight measurement on HFI bolometers. We present a semi-analytical method that exactly accounts for the scanning strategy of the instrument as well as the combination of different detectors. We use this method to propagate errors through to the CMB angular power spectra in the particular case of Planck-HFI, and to derive constraints on polarization parameters. We show that in order to limit the systematic error to 10% of the cosmic variance of the E-mode power spectrum, uncertainties in gain, polarization efficiency and detector orientation must be below 0.15%, 0.3% and 1° respectively. Pre-launch ground measurements reported in this paper already fulfill these requirements.

Item Type: Article
Date Type: Publication
Status: Published
Schools: Physics and Astronomy
Subjects: Q Science > QB Astronomy
Uncontrolled Keywords: space vehicles: instruments / techniques: polarimetric / instrumentation: polarimeters / instrumentation: detectors / cosmic microwave background / submillimeter: general
Additional Information: Pdf uploaded in accordance with publisher's policy at http://www.sherpa.ac.uk/romeo/issn/0004-6361/ (accessed 17/04/2014)
Publisher: EDP Sciences
ISSN: 0004-6361
Date of First Compliant Deposit: 30 March 2016
Last Modified: 04 Jun 2017 04:09
URI: http://orca.cf.ac.uk/id/eprint/33683

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