Changes
/* Important Notes */
In going from the raw 2D images to the 1D extractions produce by the QL Tool:
* The x axis is flipped so that increasing wavelength runs in the same direction as increasing x
* The spectra are then trimmed to remove overscan, etc.
== For IRAF users ==
Since most observers seem to have their own scripts from the old version of the spectrograph, the easiest way to reduce the data is to use the QL wavelength calibrated outputs as a reference for an IRAF reduction of the raw data.
i.e.
* Perform all the pre-processing steps as you would normally on the raw 2D data.
* When you are ready to wavelength calibrate an arc, do so as follows:
** Use the QL output as a reference. For example, a useful way is to plot the ascii wavelength solution in some interactive plotting window, like python.
** Then simply, select a few bright, well-spaced lines, hover the cursor over them, and read off the wavelength coordinate.
** Now, run IRAF - twodspec - identify on the corresponding raw 2D image. Select the same line and input its wavelength as just read off the plot. The solution is good to within a couple of Angstroms, and there are sufficient lines in the arcs that this should work well.
** Repeat for several lines.
** When happy, automatically add all the lines (press "l").
=== Advanced notes for users wishing to code up their own routines using these output files ===
* The spectra are then trimmed to remove overscan, etc.
The exact values for these are stored in:
"badMin1": 2145, <br />
in python 0-based numbering.<br />
