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<H3><A NAME="SECTION00845200000000000000">
CTRANS/ROMAFOT</A>
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<TT>CTRANS/ROMAFOT</TT>
<FONT SIZE="-1"><TT>int_tab [base_1] [base_2] [pol_deg]</TT></FONT>
<P>
This command uses the two tables generated by <TT>CBASE/ROMAFOT</TT> and
derives the analytical transformation to pass from coordinates on
``frame 1'' to coordinates on ``frame 2''.
If the transformation is considered satisfactory by the operator
(e. g. if the rms is of the order of a few tenths of a pixel or better),
the command changes the coordinates on the <I>intermediate table</I> in
order to use these as inputs in the next program frame.
In practice, after having completed reductions on the first frame,
one should copy the intermediate table and transform it.
If the transformation produces a rms larger than a few tenths of a pixel,
this means that a mismatching exists on the objects selected with
<TT>CBASE/ROMAFOT</TT>. In some cases a high rms could indicate the
necessity of an higher polyminal order (``<I>N</I>''), for the analytical
transformation, provided that more than
<BR><P></P>
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<!-- MATH: \begin{displaymath}
{N^{2}+3N+2 \over 2}
\end{displaymath} -->
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objects are available for the base.
<P>
At this point it could be useful to check the transformation
with the command
<BR> <TT>ANALYSE/ROMAFOT</TT>. In this case the <I>new</I>
frame and the intermediate table just transformed must be used and
the keys <I>D1, D2... Dk</I> will allow the display of objects with
the old parameters (height, <IMG
WIDTH="44" HEIGHT="72" ALIGN="MIDDLE" BORDER="0"
SRC="img235.gif"
ALT="$\beta$">
and so on) on the new image.
<P>
With the key <I>L</I>, in addition, it is possible to determine
the approximate central intensity of the star and the associate sky
luminosity. These values are useful to adjust the parameters in
input with the command
<P>
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<ADDRESS>
<I>Petra Nass</I>
<BR><I>1999-06-15</I>
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