Difference between revisions of "TOI processing LFI"
(Created page with '==OVERVIEW== The first step in data analysis is the correction of the ADC non linearities. ==COMPUTATION== ==APPLICATION== For each of the 44 LFI diodes there is the correspo…') |
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| − | == | + | ==Overview== |
| − | + | ==ADC Correction== | |
| − | == | + | ===Computation=== |
| − | == | + | ===Application=== |
For each of the 44 LFI diodes there is the corresponding object in the Database. Each object contains 4 columns: the input voltages coming from the sky channel and the corresponding linearized output, the input voltages coming from the reference channel and the corresponding linearized output. | For each of the 44 LFI diodes there is the corresponding object in the Database. Each object contains 4 columns: the input voltages coming from the sky channel and the corresponding linearized output, the input voltages coming from the reference channel and the corresponding linearized output. | ||
Data loaded by the module are used to initialize two different interpolator using CSPLINE and the functions from gsl ([http://www.gnu.org/software/gsl/ GNU Scientific Libraries]) libraries. The interpolators are then used to correct each sample. | Data loaded by the module are used to initialize two different interpolator using CSPLINE and the functions from gsl ([http://www.gnu.org/software/gsl/ GNU Scientific Libraries]) libraries. The interpolators are then used to correct each sample. | ||
| + | |||
| + | ==Spikes Removal== | ||
| + | |||
| + | ===Computation=== | ||
| + | |||
| + | ===Application=== | ||
| + | |||
| + | ==Gaps Filling== | ||
| + | |||
| + | ==Gain Modulation Factor== | ||
| + | |||
| + | ==Diode Combination== | ||
| + | |||
| + | ==Planet Flagging== | ||
| + | |||
| + | ==Photometric Calibration== | ||
| + | |||
| + | ==Noise Estimation== | ||
| + | |||
| + | ===Fitting the Spectra=== | ||
| + | |||
| + | ===The Final Noise Parameter=== | ||
Revision as of 14:52, 16 October 2012
Contents
Overview[edit]
ADC Correction[edit]
Computation[edit]
Application[edit]
For each of the 44 LFI diodes there is the corresponding object in the Database. Each object contains 4 columns: the input voltages coming from the sky channel and the corresponding linearized output, the input voltages coming from the reference channel and the corresponding linearized output.
Data loaded by the module are used to initialize two different interpolator using CSPLINE and the functions from gsl (GNU Scientific Libraries) libraries. The interpolators are then used to correct each sample.
Spikes Removal[edit]
Computation[edit]
Application[edit]
Gaps Filling[edit]
Gain Modulation Factor[edit]
Diode Combination[edit]
Planet Flagging[edit]
Photometric Calibration[edit]
Noise Estimation[edit]
Fitting the Spectra[edit]
The Final Noise Parameter[edit]
analog to digital converter
(Planck) Low Frequency Instrument
