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• Need a way to compute W quickly, using something like GRISMCONF
• Requires good estimates of the dispersed continuum of each sources (to remove contamination and continuum in each 2D stamp)
• The previous trade-off only stems from me wanting to use as much a-priori information as possible. Since I have deep imaging and a good idea of the continuum level of these sources and use it to remove contamination, I also use it to remove the continuum level in the source of interest. What remains is therefore just the footprint of the various emission lines. However, it is possible to generalize MAP2D into MAP3D, where we do not subtract the contamination and solve for as many discrete wavelengths as we have bins in the resulting images (i.e. 25A bins from 8000 to 11500A for G102). The issue with the later is that we still have to identify the lines in the 3D IFU cube and solving for everything increases the computation time and artifact creation (think of it as spaxel leakage as flux is distributed in adjacents spaxels and still allows the observations to be reproduced).