These blotted images will act as estimates of cosmic ray free images to be compared to the input data. The BLOTed images serve as cosmic ray free comparisons to the original images. E. Scale the images by the image exposure time. This step is necessary to help estimate errors caused by blurring in the median process and in the input shifts. This task compares the original images to their blotted counterparts.
Any significant differences are flagged as bad pixels in the mask it creates.
This task iterates to find bad pixels adjacent to pixels it has already flagged as bad. The gain and read noise are needed because the task models the noise across the chip. A better way is in the works. The defaults work well for a first pass but you will want to experiment and see just what is being flagged in the cr masks. H. Final Masks.