The mock data is a snapshots of large N-body simulation of the globular cluster M4 are available here. Full lists of data for all particles (mass, position, velocity, stellar type, stellar radius, V magnitude, B-V colour) are given at almost 400 instants in the lifetime of the model. The simulation is described in this paper http://arxiv.org/abs/1409.5597, which should be cited when making use of this data.

We selected the snapshot at t = 12023.9 Myr. A distance modulus of 11.35 mag was adopted (i.e. D=1862.1 pc). The cluster properties are:

1. Mtot = 69144.5 M_sun
2. L_V = 35547.1 L_V_sun
3. M/L_V = 1.95 Msun/L_V_sun
4. <m> = 0.495 Msun
5. r_h = 3.14 pc
6. r_eff = 1.43 pc
7. N neutron stars = 130
8. N black holes = 2
9. Mass in remnants = 27176.4 Msun

(We assume that radial/LOS velocities are available for all stars brighter than V=15 (N=1143).)

We do the comparison in 3 steps:

1. Surface brightness profile + RVs
2. Surface brightness profile + RVs + PMs
3. Surface brightness profile + RVs + PMs + Gaia

The data for the 3 fitting steps :

1. Step 1:
   1. Surface brightness: m4_sb.dat.gz
   2. Discrete LOS velocities: m4_rv.dat.gz
   3. LOS velocity dispersion profile: m4_rv_disp.dat.gz
2. Step 2:
   1. Discrete proper motions: m4_pm_mock.dat.gz
   2. Proper motion dispersion profiles: m4_pm_disp_mock.dat.gz
3. Step 3:
   1. Gaia proper motions:
   2. Gaia proper motion dispersion profiles:

For methods that allow it, you can also use constraints from a mock observed mass function at a projected radius of 300 arcseconds from the centre: m4_mass_function.tab.gz

A number density profile for stars brighter than the main-sequence turnoff (V < 17 mag; corresponding to a turnoff mass of 0.82 solar masses) is also available (m4_number_density.dat.gz). This can be used as an alternative/complement to the surface brightness profile.

The mass profile in projection and the $M/L_V$ ratio in projection can be found here:

1. m4_sigma.dat.gz