Most of the rest of this Section consists of an annotated example of how to proceed from a raw echelle image to a wavelength-calibrated single merged spectrum.
Assume that you have images of a continuum source such as a bright, smooth spectrum star or an quartz lamp taken with SL MIN (for tracking the echelle orders), of the ThAr lamp (for wavelength calibration) and of your object. In some cases the object spectra are sufficiently well exposed and free of discontinuities to allow direct order tracking. In such cases there will be no need for a separate continuum spectrum.
These files are in your current directory and are called:
CONTRAW.DST continuum ARCRAW.DST arc OBJRAW.DST object
In what follows it will be useful to refer to Figure 
.