PI: Antonio Sollima
Co-I: Alice Zocchi
Other active participants: Mark Gieles, Vincent Henault-Brunet, …

Questions to address:

1. How different are the fits when considering: 1) all stars and 2) only visible stars?
2. Is it better to consider luminosity weighted profiles, or number density profiles?
3. How much can we do with 2 velocity components instead of 1 (i.e. with Gaia data)?

(Simulations ran and kindly made available by Holger Baumgardt)

Here we consider 2 clusters which are slightly more realistic:

1. IC: King (1966) W_0 = 5 model, N = 131072, Kroupa (2001) mass function between 0.1-15 Msun (no black-holes).
2. No primordial binaries, no central black hole, circular orbit in logarithmic halo with V = 220 km/s.
3. Z = 0.001
4. Stellar evolution and mass-loss according to Hurley et al. (2000, 2002)
5. Two Galactocentric radii: 8.5 kpc and 15 kpc.

Below are 2 snapshots at an age of roughly 10 Myr, 100 Myr, 1Gyr and 12 Gyr. The columns are the same as in Challenge 2.

1. w05_n131k_rg8.5_feh-0.0_t10.gz UPDATED! Thursday August 22
2. w05_n131k_rg8.5_feh-0.0_t100.gz UPDATED! Thursday August 22
3. w05_n131k_rg8.5_feh-0.0_t1000.gz UPDATED! Thursday August 22
4. w05_n131k_rg8.5_feh-0.0_t12000.gz
5. w05-n131k_rg15_feh-0.0.t10.gz NEW! Tuesday August 20
6. w05-n131k_rg15_feh-0.0.t100.gz NEW! Tuesday August 20
7. w05-n131k_rg15_feh-0.0.t1000.gz NEW! Tuesday August 20
8. w05_n131k_rg15_feh-0.0_t12000.gz

The definition of the stellar types (KSTAR) used in the NBODY6 snapshots can be found in the Appendix.

As another source of mock data, snapshots from a 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 the paper “Towards an N-body model of the globular cluster M4”, submitted to MNRAS (http://arxiv.org/abs/1409.5597), which should be cited when making use of this data.