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

D. Maino¹ - C. Burigana² - M. Maltoni^2,3,4 - B.D. Wandelt⁵ - K.M. Górski^5,6,7 - M. Malaspina² - M. Bersanelli⁸ - N. Mandolesi² - A.J. Banday⁹ - E. Hivon¹⁰

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.

Abstract:

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