Difference between revisions of "Map-making"
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* We remove the reconstruction above from each ring of data. | * We remove the reconstruction above from each ring of data. | ||
* We then make maps as described in section ????? | * We then make maps as described in section ????? | ||
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| + | == Far Sidelobe Correction == | ||
== Map validation == | == Map validation == | ||
[[Category:Data processing]] | [[Category:Data processing]] | ||
Revision as of 05:32, 15 October 2012
Contents
Introduction
Flux calibration
Noise properties
Zodi correction
Zodiacal Emission is removed from the 353, 545 and 857 GHz channels. It is described in ?????, but a synopsis of the procedure is as follows:
- During each survey, a large fraction of the sky has observations which all fall within a week of each other. That is, during a single survey, most pixels are observed during a short, well-defined period. The contribution from Zodiacal Emission to the total brightness seen, then, is well defined.
- We use the the COBE model of the Zodiacal Light to make predictions for this emission.
- We fit the survey difference maps with these model templates to estimate the emissivity of each component at the Planck wavelengths.
- We reconstruct the full mission using the combination of the COBE geometric model with the emissivities determined above.
- We remove the reconstruction above from each ring of data.
- We then make maps as described in section ?????
