When identifying the pixel data in the measurement images for the flexible model fitting the RA/Dec positions of all sources are projected into pixel coordinates of each measurement image.
The measurement images have non-linear astrometric solutions, which can result in an error in WCSLIB if the projection does not have a unique solution, and SE++ just stops (see #554). This happens only for sources far off the boundaries of a the measurement images and we need to find ways to avoid these breaks.
When identifying the pixel data in the measurement images for the flexible model fitting the RA/Dec positions of all sources are projected into pixel coordinates of each measurement image.
The measurement images have non-linear astrometric solutions, which can result in an error in WCSLIB if the projection does not have a unique solution, and SE++ just stops (see #554). This happens only for sources far off the boundaries of a the measurement images and we need to find ways to avoid these breaks.