Aberrations

Gaertner, Johannes A.; Baltrušaitis, Jurgis

doi:10.2307/40098974

Cited by 1 publication

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“…Note also that this ‘destriping’ method handles the polarization signal seamlessly, avoiding the technicalities involved in estimating offsets from ring intersections for polarized detectors (Revenu et al 2000). Removing the n =0 and l =0 modes from the analysis also neatly solves the problem of degeneracy that arises if the experiment is insensitive to the monopole – this situation may arise for the Planck HFI as the favoured readout electronic system is insensitive to very low frequencies (Gaertner et al 1997).…”

Section: Discussionmentioning

confidence: 99%

Harmonic analysis of cosmic microwave background data -- II. From ring-sets to the sky

Challinor¹,

Mortlock

Leeuwen

et al. 2002

Monthly Notices of the Royal Astronomical Society

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A B S T R A C TDespite the fact that the physics of the cosmic microwave background anisotropies is most naturally expressed in Fourier space, pixelized maps are almost always used in the analysis and simulation of microwave data. A complementary approach is investigated here, in which maps are used only in the visualization of the data, and the temperature anisotropies and polarization are only ever expressed in terms of their spherical multipoles. This approach has a number of advantages: there is no information loss (assuming a band-limited observation); deconvolution of asymmetric beam profiles and the temporal response of the instrument are naturally included; correlated noise can easily be taken into account, removing the need for additional 'destriping'; polarization is also analysed in the same framework; and reliable estimates of the spherical multipoles of the sky and their errors are obtained directly for subsequent component separation and power spectrum estimation. The formalism required to analyse experiments which survey the full sky by scanning on circles is derived here, with particular emphasis on the Planck mission. A number of analytical results are obtained in the limit of simple scanning strategies. Although there are non-trivial computational obstacles to be overcome before the techniques described here can be implemented at high resolution, if these can be overcome the method should allow for a more robust return from the next generation of full-sky microwave background experiments. (FvL) 1 http://map.gsfc.nasa.gov/ 2 http://astro.estec.esa.nl/Planck/ Mon. Not. R. Astron. Soc. 331, 994-1010 q 2002 RAS 3 Our convention for the Euler angles a, b and g are such that the rotation D(a, b, g) actively rotates by g about s z , followed by b about s y , and finally by a about s z again. All rotations are right-handed. See Brink & Satchler (1993), whose conventions we follow, for a discussion of the several alternatives that appear in the literature.

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