This project is not yet finished. The project is outlined in this Overleaf document (editable at this link):
https://www.overleaf.com/6955685585cxpvzqqjypkz
The current task of the project is to determine two "nuisance" parameters in the fit (two of the parameters in Table 1): the binning radius, R_{bin}, and the grid density, R_{grid}. I think we should use five different values for R_{bin}: 100, 150, 200, 250, and 300 Mpc. These are chosen, as they span the general scale of superclusters/voids at the lower end and are the size of a PanStarrs medium deep field at the maximum redshift of z = 0.8 at the high end.
Ideally, R_{grid} would be arbitrarily small (we would do the fit in the entire sky). But that is not practically feasible. Instead, we should find the values of R_{grid} at which the SNe 3d peculiarity fits converge. In other words, we should run the full SNe 3 peculiarity effects at a range of R_{grid} values for each of the R_{bin} values, and determine at which point making R_{grid} better (smaller) ceases to matter. This is a somewhat lengthy process. We are partially done.
Once these convergence values are determined, we should run a series (~1000) of chains with data randomized. We keep track of the data in this sheet:
Green cells in the sheet are chains that have been completed.
Yellow cells are chains that have been executed on the cluster, but not completed.
Red cells are chains that we think should be run, but have not yet been started.
Because the number of seed points can be quite large before we achieve convergence in R_{grid}, we divide the sky into a certain number of slices on the sky. Experimentation shows that ~180 slices is a good number. Therefore, we have suggested that