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In order to produce a set of analysed data, you
first have to reduce the data into a format in which you can use
the fitting procedure. This means reducing the data, calibrating
the variations in intensity and position within the array, and
outputting the results of this to a file. In order to correct
an object file for analysis, you must apply the following corrections
to the raw data:
1) Use a flat field to remove the variations in
any image associated with the array itself
2) Use the Sky back ground to subtract the effects
of sky emission and absorption on the data
3) Use both arc and star lines to allow the correction
of the data associated with bends and flexures in the array
4) Use the star lines in order to correct for
remaining intensity variations as a function of wavelength, and
to flux calibrate the data, that is, to calculate the true intensity
of the lines by comparing it with the known value for the star
This is completed in the following steps:
Phase 1: Initial
Reduction
Phase 2: Flat-fielding
Phase 3: Data Reduction
Phase 4: Wavelength Position
Phase 5: Flux Calibration
Phase 6: Spectral Location
Phase 7: Spectral Fitting
Phase 8: Mapping
X-order 1: Reduction
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