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<H3><A NAME="SECTION003432100000000000000">&#160;</A>
  <A NAME="irac2:standard-construction">&#160;</A>
<BR>
Standard construction
</H3>
  There are two ways to produce flat fields for use with IR data. The
  standard method is to take 'LAMP ON' and 'LAMP OFF' exposures of the
  calibration spot on the telescope dome. The 'LAMP ON' exposure
  contains light from both the calibration lamp, which should provide
  the even illumination needed for the flat field, together with
  potentially uneven illumination from the telescope and instrument
  environments. To retain only the even calibration illumination, the
  ``LAMP OFF'' image must be subtracted from the ``LAMP ON'' image. This
  subtraction also removes the bias pattern from the flat field image.

<P>
The subtracted image should then be normalised for later use as a flat
  field.

<P>
In MIDAS, you may directly use <TT>COMPUTE/IMAGE</TT> to perform 
  the subtraction. The image mean may then be calculated using
  <TT>STATISTICS/IMAGE</TT> or similar. The ``LAMP on - LAMP OFF'' image 
  can then be divided by this value using <TT>COMPUTE/IMAGE</TT> for 
  normalisation.
  Alternatively, the procedure MKFLAT/IRAC2 combines these actions.
  To improve the signal-to-noise ratio of the flat-field, a number of
  flat field images may be used together. These should be combined using
  <TT>COMBINE/CCD</TT> (see later).

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