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<H3><A NAME="SECTION003262300000000000000">
Measuring aperture</A>
</H3>
The wings of a telescopic image are due to surface scattering caused by
microroughness of polished optical surfaces, and to (usually) a much
smaller extent to scattering by dirt on the optics.
Contrary to popular mythology, atmospheric effects are quite negligible.
These wings contain some tens of per cent of the total starlight, for
typical surface quality.
If the measuring aperture varies, a varying amount of starlight will be
excluded.
Furthermore, the excluded fraction is wavelength-dependent; so the
transformation from instrumental to standard system changes.
Therefore,
the field stop, physical or synthesized, within which the measurements were
made, should always be constant.

<P>
Unfortunately, sometimes it is necessary to combine measurements made with
different field stops.
Observers should realize that this really means different instruments;
the differences are usually several per cent.
Calibration data should be taken (i.e., several stars of different colors
observed with all the apertures used) to determine the transformations between
them.

<P>
Usually, the actual aperture sizes are only approximately known.
In any case, the actual variation of the excluded energy fraction
with radius is not accurately predictable.
Therefore, it suffices to retain codes for apertures, rather than try to deal
with them quantitatively.
The code should be put in a column labelled DIAPHRAGM (the common term for the
field stop).

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