Quote:
Originally Posted by RickS
I think there are a number of different factors involved here but saturation alone is enough to explain a degree of bloat on bright stars. When the top of a star profile starts to get truncated by reaching full well depth the FWHM will increase. A diagram would help to make this clear but I don't have time to draw one right now...
Cheers,
Rick.
|
I think so Rick.
A simple experiment would be to take 2 exposures of a bright star field. One is short, say 20 seconds, the other is 10 minutes and measure the FWHM's of the same stars in each. That would reveal the short image has tighter stars I am predicting.
Greg.