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Astron. Astrophys. Suppl. Ser. 140, 383-391

The Planck-LFI instrument: Analysis of the 1/f noise and implications for the scanning strategy

D. Maino1 - C. Burigana2 - M. Maltoni2,3,4 - B.D. Wandelt5 - K.M. Górski5,6,7 - M. Malaspina2 - M. Bersanelli8 - N. Mandolesi2 - A.J. Banday9 - E. Hivon10

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1 - SISSA, International School for Advanced Studies, Via Beirut 2-4, I-34014 Trieste, Italy
2 - Istituto TeSRE, Consiglio Nazionale delle Ricerche, Via Gobetti 101, I-40129 Bologna, Italy
3 - Dipartimento di Fisica, Universitá di Ferrara, Via Paradiso 12, I-44100 Ferrara, Italy
4 - INFN, Sezione di Ferrara, Via Paradiso 12, I-44100 Ferrara, Italy
5 - TAC, Theoretical Astrophysics Center, Juliane Maries Vej 30, DK-2100 Copenhagen, Denmark
6 - ESO, European Southern Observatory, Karl-Schwarzschild Str. 2, D-85748, Garching, Germany
7 - Warsaw University Observatory, Warsaw, Poland
8 - IFC, Consiglio Nazionale delle Ricerche, Via Bassini 15, I-20133 Milano, Italy
9 - MPA, Max Planck Inst. für Astrophysik, Karl-Schwarzschild Str. 1, D-85740, Garching, Germany
10 - CalTech, California Institute of Technology, 1200 East California Boulevard, CA-91125, Pasadena, U.S.A.

Received June 4; accepted September 20, 1999


We study the impact of 1/f noise on the PLANCK Low Frequency Instrument (LFI) observations (Mandolesi et al.[1998]) and describe a simple method for removing striping effects from the maps for a number of different scanning strategies. A configuration with an angle between telescope optical axis and spin-axis just less than 90$^{\circ }$ (namely $\simeq 85^\circ$) shows good destriping efficiency for all receivers in the focal plane, with residual noise degradation $< 1-2\%$. In this configuration, the full sky coverage can be achieved for each channel separately with a 5$^{\circ }$ spin-axis precession to maintain a constant solar aspect angle.

Key words: methods: data analysis -- cosmology: cosmic microwave background -- space vehicles

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