Astron. Astrophys. Suppl. Ser.
Volume 140, Number 3, December II 1999
|Page(s)||383 - 391|
|Published online||15 December 1999|
The Planck-LFI instrument: Analysis of the noise and implications for the scanning strategy
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.
Accepted: 20 September 1999
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.
Key words: methods: data analysis / cosmology: cosmic microwave background / space vehicles
© European Southern Observatory (ESO), 1999