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<TITLE>Photometry of the Other Program Frames</TITLE>
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<H2><A NAME="SECTION00845000000000000000">
Photometry of the Other Program Frames</A>
</H2>
The procedure described above is the standard procedure and results
in an <I>independent</I> reduction of <I>each</I> frame.
However, there are cases where a different approach is more
efficient. Imagine, for instance, that several frames of the
same region in the sky had to be reduced but the frames were taken in
different seeing conditions, or at telescopes with different
pixel matching. It is useful, in this case, to <I>transfer</I> the inputs
from the frame with the best resolution to the others. The result of
this operation is to add information (number of components, for instance)
to the frames of poor quality. This procedures obviously applies also
to frames taken with different filters.
<P>
The operation requires three logical steps:
<DL COMPACT>
<DT>1.
<DD>Create a base for transformation of coordinates from frame <I>A</I>
to frame <I>B</I>;
<DT>2.
<DD>Transform the coordinates from <I>A</I> to <I>B</I>;
<DT>3.
<DD>Adjust the input (intensity, background, holes and so forth)
</DL>
<P>
These steps are accomplished by the commands <TT>CBASE/ROMAFOT</TT>,
<TT>CTRANS/ROMAFOT</TT> and <TT>ADAPT/ROMAFOT</TT>, respectively.
<P>
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<ADDRESS>
<I>Petra Nass</I>
<BR><I>1999-06-15</I>
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