Difference between revisions of "HFI/LFI joint data processing"
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| − | HFI/LFI common processing uses as basic input the maps at the | + | The HFI / LFI common processing uses as basic input the maps at the nine frequencies covered by the two instruments. |
| − | The goal is to obtain various catalogues, identify the different astrophysical components whose superposition leads to the observed sky, and | + | The goal is to obtain various catalogues, identify the different astrophysical components whose superposition leads to the observed sky, and provide a statistical characterization of the CMB, in particular through a likelihood code (of a particular theoretical <i>C</i><sub>ℓ</sub> given Planck data). |
| − | + | * [[Detector pointing| Detector pointing]] | |
| + | * [[Compact Source catalogues | Compact source catalogues]] | ||
| + | * [[Astrophysical component separation]] | ||
| + | * [[C2 | CMB power spectra and Planck likelihood code]] | ||
| − | + | [[Category:HFI/LFI joint data processing|000]] | |
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Latest revision as of 09:44, 10 July 2018
The HFI / LFI common processing uses as basic input the maps at the nine frequencies covered by the two instruments.
The goal is to obtain various catalogues, identify the different astrophysical components whose superposition leads to the observed sky, and provide a statistical characterization of the CMB, in particular through a likelihood code (of a particular theoretical Cℓ given Planck data).
(Planck) High Frequency Instrument
(Planck) Low Frequency Instrument
Cosmic Microwave background
