We should redo Clare's 2016 analysis with a 2D Gaussian fit function (see Follette-group/GAPlanetS/python/pyklip_headers.py for a nice function to do this). There might now be more datasets that meet the criteria of (a) unsaturated and (b) bright enough to have a detectable ghost. Basic questions are: (1) what is the ratio of ghost peak to star peak? (2) what is the stability of this ratio from dataset to dataset? (3) how different are the FWHM values of ghost and star? is the ghost a reasonable proxy?
We should redo Clare's 2016 analysis with a 2D Gaussian fit function (see Follette-group/GAPlanetS/python/pyklip_headers.py for a nice function to do this). There might now be more datasets that meet the criteria of (a) unsaturated and (b) bright enough to have a detectable ghost. Basic questions are: (1) what is the ratio of ghost peak to star peak? (2) what is the stability of this ratio from dataset to dataset? (3) how different are the FWHM values of ghost and star? is the ghost a reasonable proxy?