Purpose

As described in Chapter , the reduction of long slit spectra comprises three main steps:

1. Pre-reduction:
   -- removal of cosmic rays
   -- flat-fielding
   -- dark subtraction.
2. Geometric corrections:
   -- correction for distortions perpendicular to the dispersion direction ( e.g., due to differential refraction in the earth's atmosphere)
   -- determination of the dispersion curve
   -- resampling of the data to constant step in wavelength.
3. Final photometric operations :
   -- sky subtraction
   -- flux calibration.

Section is a summary of a typical session but without much explanation on the methods or general advice. First-time users may find it useful to follow it as it stands, step by step, in order to become acquainted with the plain technical operation of the available commands. Section presents the Graphical User Interface XLong. The interface XLong is a convenient way to gain visibility on the parameter values, avoid command syntax problems and understand the organisation of the context.

Note Although this Appendix is intended to be self-contained, it cannot serve as a substitute for the HELP information available for all the individual commands mentioned. Full advantage of the flexibility of the tools offered for the reduction of long slit spectra can be taken only on the basis of the command's detailed explanations in Volume A and more specifically in Chapter 6 (long-slit spectra) of Volume B.