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

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: 4 June 1999
Accepted: 20 September 1999

Abstract

We study the impact of noise on the Planck Low Frequency Instrument (LFI) observations (Mandolesi et al.  ) 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° (namely ) shows good destriping efficiency for all receivers in the focal plane, with residual noise degradation . In this configuration, the full sky coverage can be achieved for each channel separately with a 5° spin-axis precession to maintain a constant solar aspect angle.