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\@writefile{lof}{\contentsline {figure}{\numberline {1}{\ignorespaces   This is an example of the difference that good guiding can make. See how nice and round the star in the image on the left is? That image was properly guided, as opposed to the image on the right where the star looks like more like a loaf of bread!}}{3}}
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\@writefile{lof}{\contentsline {figure}{\numberline {3}{\ignorespaces  this is an example of what the settings for imcombine look like. The settings are appropriate for combining flat field images.}}{7}}
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\@writefile{lof}{\contentsline {figure}{\numberline {4}{\ignorespaces  This is an example of a flat field image. Notice the doughnut-shaped shadows that come from dust on the optics. You can also see that some pixels are more sensitive to light than others, and that there is less light around the edges. The difference between the most sensitive and the least sensitive pixels is about 5\%. }}{9}}
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\@writefile{lof}{\contentsline {figure}{\numberline {5}{\ignorespaces  This is an example of how IRAF measures the brightness of a star. The light from the star is added up from the pixels that are within the smaller circle, and the pixels that are between the smaller and larger circle are used to determine the background sky brightness. You can see that even where there are no stars, there is some light. This light does not come from the star we want to measure, so it has to be removed.}}{10}}
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\@writefile{lof}{\contentsline {figure}{\numberline {6}{\ignorespaces These are the settings for the qphot command.}}{11}}
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\@writefile{lof}{\contentsline {figure}{\numberline {7}{\ignorespaces  This is an example of a ``folded'' light curve. These observations may have been taken years apart, but because we plot the variations as a function of phase and not actual time, we can see them all on one plot. }}{13}}
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