The final algorithm can be updated in the deblend module of lsst-ts/ts_wep package. The code there does not work at all for amplifier images. One of the problem is the low signal-to-noise ratio. In addition, we also need to consider the overlap of defocused bright star and galaxy. For the corner wavefront sensor, the vignette is also a problem.
The final algorithm can be updated in the
deblend
module of lsst-ts/ts_wep package. The code there does not work at all for amplifier images. One of the problem is the low signal-to-noise ratio. In addition, we also need to consider the overlap of defocused bright star and galaxy. For the corner wavefront sensor, the vignette is also a problem.