SpeX Data Processing


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