Volume 373, Number 1, July I 2001
|Page(s)||345 - 358|
|Section||Numerical methods and codes|
|Published online||15 July 2001|
PLANCK LFI: Comparison between Galaxy Straylight Contamination and other systematic effects
Istituto TeSRE, Consiglio Nazionale delle Ricerche, via Gobetti 101, 40129 Bologna, Italy
2 Oss. Astr. Trieste, via G.B. Tiepolo 11, 34131 Trieste, Italy
3 ESO, European Southern Observatory, Karl-Schwarzschild Str. 2, 85748 Garching, Germany
4 Warsaw University Observatory, Warsaw, Poland
5 Dipartimento di Fisica, Università di Milano, and IFC/CNR, via Celoria 16, 20133 Milano, Italy
6 Department of Physics, Princeton University, Princeton, NJ 08544, USA
7 Instituto de Física Corpuscular -CSIC/UVEG, Edificio Institutos de Paterna, Apt. 22085, 46071 Valencia, Spain
8 Observational Cosmology, California Institute of Technology, MS 59-33, CA 91125 Pasadena, USA
9 IPAC, California Institute of Technology, MS 100-22, CA 91125 Pasadena, USA
Corresponding author: C. Burigana, firstname.lastname@example.org
Accepted: 14 March 2001
The straylight contamination due to the Galactic emission (GSC, Galaxy Straylight Contamination) entering at large angles from the antenna centre direction may be one of the most critical sources of systematic effects in observations of the cosmic microwave background (CMB) anisotropies by future satellite missions such as Planck and MAP. While future accurate measurements of the real antenna pattern are necessary for a firm evaluation of this effect, on the basis of the currently available optical simulations we are able to produce simulated data useful for the development of data analysis methods and the optimization of the optical design. For the Low Frequency Instrument (LFI), the GSC is expected to be particularly crucial at the lowest frequency channels. We describe here different methods to evaluate the impact of this effect and compare it with other systematics of instrumental and astrophysical origin. The results are presented in terms of simulated data streams and maps, Fourier series decomposition and angular power spectrum. The contributions within a few degrees from the beam centre dominate the GSC near the Galaxy plane. The antenna sidelobes at intermediate and large angles from the beam centre dominate the GSC at medium and high Galactic latitudes. We find a GSC peak at ∼15 μK and a GSC angular power spectrum above that of the white noise for multipoles , albeit smaller than that of CMB anisotropies by a factor larger than ∼10. At large multipoles, the GSC affects the determination of CMB angular power spectrum significantly less than other kinds of instrumental systematics, such as main beam distortions and noise. Although the GSC is largest at low Galactic latitudes, the contamination produced by far pattern features at medium and high Galactic latitudes, peaking at ~4 μK, has to be carefully investigated, because the combination of low amplitude of Galaxy emission in those regions with the extremely good nominal Planck sensitivity naturally makes high Galactic latitude areas the targets for unprecedentedly precise estimation of cosmological CMB anisotropy. This paper is based on Planck LFI activities.
Key words: cosmology: cosmic microwave background / Galaxy: general / space vehicles / telescopes / methods: data analysis
© ESO, 2001
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