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

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<H3><A NAME="SECTION002519100000000000000">
The Simplest Case</A>
</H3> 

<P>
This paragraph shows the very simplest possible example of how to do the
relative calibration of a CCD-frame. It is assumed that frames are only taken
in a single filter (R in this case). The frames available are the following: 
<UL>
<LI>Darks
  <DL COMPACT>
<DT>
<BR>
<DD>DARK01    is a 20 minute frame taken before/after observing
<DT>
<BR>
<DD>DARK02    <I>dito</I>
<DT>
<BR>
<DD>DARK03    <I>dito</I>
<DT>
<BR>
<DD>DARK04    <I>dito</I>
  </DL>
<LI>Flats
  <DL COMPACT>
<DT>
<BR>
<DD>FLATR1   20 sec dome flat in R-filter
<DT>
<BR>
<DD>FLATR2   <I>dito</I>
<DT>
<BR>
<DD>FLATR3   <I>dito</I>
  </DL>
<LI>Data
  <DL COMPACT>
<DT>
<BR>
<DD>N5126R   20 minute exposure of NGC&nbsp;5126
<DT>
<BR>
<DD>N7794R   20 minute exposure of NGC&nbsp;7794
  </DL></UL>In order to process these frames, the following commands would be executed.<BLOCKQUOTE>
<TT>AVERage/IMAge  DARKAV = DARK01,DARK02,DARK03,DARK04
<BR>
AVERage/IMAge  FLATAV = FLATR1,FLATR2,FLATR3
<BR>
COMPute/IMAge  DENOM = FLATAV-DARKAV
<BR>
COMPute/IMAge  N5126RF = (N5126R-DARKAV)/DENOM
<BR>
COMPute/IMAge  N7794RF = (N7794R-DARKAV)/DENOM</TT></BLOCKQUOTE>The first two commands compute the simple averages of the dark and flat field
images. The third command computes the dark subtracted average flat field.
The final two commands perform the flat fielding of the data frames. Note that
there has been no correction for bad columns in either the flat field, the 
dark frames or the data frames. The next example shows how to do this.

<P>
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<ADDRESS>
<I>Petra Nass</I>
<BR><I>1999-06-15</I>
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