Planck pre-launch status: High Frequency Instrument polarization calibration

被引：81

作者：

Rosset, C. ^{[1
,5
]}

Tristram, M. ^{[1
,11
]}

Ponthieu, N. ^{[2
]}

Ade, P. ^{[3
]}

Aumont, J. ^{[2
,11
]}

Catalano, A. ^{[4
,5
]}

Conversi, L. ^{[16
]}

Couchot, F. ^{[1
]}

Crill, B. P. ^{[6
,9
]}

Desert, F. -X. ^{[7
]}

Ganga, K. ^{[5
]}

Giard, M. ^{[8
]}

Giraud-Heraud, Y. ^{[5
]}

Haissinski, J. ^{[1
]}

Henrot-Versille, S. ^{[1
]}

Holmes, W. ^{[9
]}

Jones, W. C. ^{[6
,9
,14
]}

Lamarre, J. -M. ^{[4
]}

Lange, A. ^{[6
,9
]}

Leroy, C. ^{[2
,8
]}

Macias-Perez, J. ^{[7
]}

Maffei, B. ^{[10
]}

de Marcillac, P. ^{[2
]}

Miville-Deschenes, M. -A. ^{[2
]}

Montier, L. ^{[8
]}

Noviello, F. ^{[2
]}

Pajot, F. ^{[2
]}

Perdereau, O. ^{[1
]}

Piacentini, F. ^{[12
]}

Piat, M. ^{[5
]}

Plaszczynski, S. ^{[1
]}

Pointecouteau, E. ^{[8
]}

Puget, J. -L. ^{[2
]}

Ristorcelli, I. ^{[8
]}

Savini, G. ^{[3
,15
]}

Sudiwala, R. ^{[3
]}

Veneziani, M. ^{[5
,12
]}

Yvon, D. ^{[13
]}

机构：

[1] Univ Paris 11, CNRS, LAL, Lab Accelerateur Lineaire, F-91405 Orsay, France

[2] Univ Paris 11, CNRS, IAS, Inst Astrophys Spatiale, F-91405 Orsay, France

[3] Cardiff Univ, Astron & Instrumentat Grp, Cardiff, S Glam, Wales

[4] Observ Paris, CNRS, LERMA, F-75014 Paris, France

[5] Univ Paris Diderot, APC Astroparticule & Cosmol, F-75205 Paris 13, France

[6] CALTECH, Observat Cosmol, Pasadena, CA 91125 USA

[7] CNRS, LAOG, Astrophys Lab, Observ Grenoble, Grenoble, France

[8] CNRS, CESR, F-31038 Toulouse 4, France

[9] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA

[10] Univ Manchester, JBCA, Sch Phys & Astron, Manchester M13 9PL, Lancs, England

[11] CNRS, LPSC, Lab Phys Subatom & Cosmol, Grenoble, France

[12] Univ Roma La Sapienza, Dipartimento Fis, I-00185 Rome, Italy

[13] CEA, Serv Phys Particules, Saclay, France

[14] Princeton Univ, Dept Phys, Princeton, NJ 08544 USA

[15] UCL, Opt Sci Lab, London WC1E 6BT, England

[16] European Space Astron Ctr, Villanueava De La Canada 28691, Madrid, Spain

来源：

ASTRONOMY & ASTROPHYSICS | 2010年 / 520卷

关键词：

space vehicles: instruments; techniques: polarimetric; instrumentation: polarimeters; instrumentation: detectors; cosmic microwave background; submillimeter: general; PROBE WMAP OBSERVATIONS; POWER SPECTRA; MICROWAVE; TEMPERATURE; PARAMETERS;

D O I：

10.1051/0004-6361/200913054

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

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 (Delta P/T-cmb similar to 4 x 10(-6) for P either Q or U and T-cmb similar or equal to 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 l similar 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 degrees respectively. Pre-launch ground measurements reported in this paper already fulfill these requirements.

引用

页数：12

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