There is a slight difference in the flux outputted between the old (v2.2.0) and new (branch reimplement_cr_reject) version of the PLP where the flux/counts on the reduced data in the new version is about 3-4% larger than the old version. It is not entirely clear why. Below is an image of a .spec.fits file of the same reduced A0V star spectrum with the new PLP divided by the old PLP. It seems to vary across the detector. It might have something to do with how flats are treated or how the background is treated. We will need to look into this further. Relative flux calibration will negate this effect so it is not much of a concern science wise.
There is a slight difference in the flux outputted between the old (v2.2.0) and new (branch reimplement_cr_reject) version of the PLP where the flux/counts on the reduced data in the new version is about 3-4% larger than the old version. It is not entirely clear why. Below is an image of a .spec.fits file of the same reduced A0V star spectrum with the new PLP divided by the old PLP. It seems to vary across the detector. It might have something to do with how flats are treated or how the background is treated. We will need to look into this further. Relative flux calibration will negate this effect so it is not much of a concern science wise.