Results of the fits of MW globular clusters using GCfit

• clusters/

  • NGC*/
    • Output files from all sampling runs, for each cluster (see below)
    • Parameter posteriors, marginal distributions, black hole probability distributions, kinematic profiles, cumulative mass profiles and mass function confidence intervals, for each cluster
    • Core collapsed clusters are also shown without BHs under no_BHs/

• parameters/

  • Summary (machine-readable) table of all best-fitting parameters with statistical uncertainties
  • All figures represent the final sample of clusters as used in paperI (i.e. including ω-cen, with bad fits removed and with fixed core-collapsed clusters), after refits for paperII. See the papers (or paper{I,II}_figures/) for cleaner plots.
  • comparisons/
    • Distance, remnant fraction, mass, half-mass radius and BH mass comparisons with various literature values
  • distributions/
    • Violin plots of distributions of all parameters, for all clusters
  • relations/
    • Relationships between all parameters, and all parameters with dynamical age, remaining mass fraction, and orbital parameters

• thesis_figures/

  • All figures from the MSc thesis corresponding to this work
  • These are most likely out of date, but shown here for posterity

• paperI_figures/

  • All figures from paperI (Multimass modelling of Milky Way globular clusters I. Implications on their stellar initial mass function above 1 Msun)

• Gaia_profiles

  • All extracted Gaia EDR3 proper motion dispersion profiles

Using sampler output files

The sampler outputs from all of the fitting runs, including parameter chains, likelihoods, priors, nested bounds, etc., are available for each cluster, as HDF5 files (clusters/NGC*_sampler.hdf).

For more instructions and information on using these outputs and recreating the models, see the GCfit documentation.