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eso-midas-doc-13SEPpl1.2-3.mga5.i586.rpm

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<H2><A NAME="SECTION003011000000000000000">
Purpose</A>
</H2>

<P>
As described in Chapter <A HREF="node676.html#spectral-data">L</A>, the reduction of 
long slit spectra comprises three main steps:

<P>
<DL COMPACT>
<DT>1.
<DD>Pre-reduction: <BR> 
- removal of cosmic rays <BR>
- flat-fielding <BR>
- dark subtraction. 
<DT>2.
<DD>Geometric corrections: <BR>
- correction for distortions perpendicular to the dispersion direction 
(<I>e.g.</I>, due to differential refraction in the earth's atmosphere) <BR>
- determination of the dispersion curve <BR>
- resampling of the data to constant step in wavelength. 
<DT>3.
<DD>Final photometric operations : <BR> 
- sky subtraction <BR> 
- flux calibration. 
</DL>
<P>
Section <A HREF="node501.html#c-book">G.3</A> 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 <A HREF="node521.html#ap:XLong">G.4</A> 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.

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<BLOCKQUOTE>
<DIV ALIGN="CENTER">
<B>Note</DIV>
<I>Although this Appendix is intended to be self-contained, it cannot serve 
as a substitute for the <TT>HELP</TT> 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.</I></B></BLOCKQUOTE>
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<ADDRESS>
<I>Petra Nass</I>
<BR><I>1999-06-15</I>
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