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

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<H2><A NAME="SECTION00847000000000000000">
Big Pixels</A>
</H2>
   This problem is examined in Buonanno and Iannicola, 1989.
   In short, ROMAFOT performs the best fit by comparing a given pixel 
   to the value of the PSF at the centre of the pixel. This approximation 
   is valid if the pixel size is small compared with the scale length of 
   the point images. If <I>R</I> is the ratio between the FWHM of the PSF 
   and the pixel size, then a value of <IMG
 WIDTH="35" HEIGHT="20" ALIGN="BOTTOM" BORDER="0"
 SRC="img241.gif"
 ALT="$R\sim 1.5$">
is the limit of validity 
   of the quoted approximation and, correspondingly, the limit beyond 
   which we enter in the regime of <I>big pixels</I>. With the commands 
   below the integral of the PSF over the pixel area is computed 
   via the Gauss - Legendre integration formulae which are characterized 
   by a high precision for a correspondingly small number of subpixels 
   where the PSF must be calculated.

<P>
Since the number of subpixels depends on the intensity of the star, 
   on the local gradient of the PSF and so on, two commands are used.
   The first command prepares a file where the subpixel values are computed
   according to the different parameters of the problem (aperture of the 
   telescope, exposure time, seeing, required accuracy, magnitude of the 
   star, distance of the pixel from the centre of the star and so forth).
   The second command performs the non - linear fitting by comparing the 
   integral of the PSF over the subpixel values.

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