These DFs are calculated for different potentials (`Cusp' or `Core'), different light profiles (`Plum' or 'Nonplum'; but note that even the `Plum' case is not quite Plummer as it has an inner slope with power-law index 0.1 instead of 0), and different velocity anisotropy profiles (`Iso', 'OM', `Tan' for isotropic, Osipkov-Merritt and constant tangential).

• See Matthew Walker's README for explanations of the columns of the first eight and last two mock datasets.
• For the single component models, versions with velocity errors are included in separate *_err.dat files. The velocity errors are applied to vx,vy,vz and assumed to be Gaussian of width 2km/s. Please use the files WITH velocity errors as default.
• The single component models are also available with different sampling. In priority order, please run:
  • Full sampling (10000 stars);
  • 1000 stars, model _0
  • 100 stars, model _0
  • And, if feasible 1000 star models _1 → _4 and 100 star models _1 → _9
• The tangential models are described in another README. (Note: the alpha values provided in this file are 1/alpha as defined in the readme above for the other spherical models.)
• For the split component models, velocity errors, contamination and metallicity distribution functions for each component have are all included in the data files. See the above .pdf for further details. Included are the original mocks from Matt Walker and two more for each of the cored and cusped cases :: one where the mean Mg of the two populations is separated by 0.35dex (_mgsepsamll.dat); and one where it is by 0.6dex (_mgseplarge.dat). Please run these using all available stars.
• In all cases units are kpc, km/s.

In order to enable straightforward comparisons, please test first using the projection along the Z-axis. Projections along X- and Y- axes can subsequently be used for 'independent' realisations.