====== GC2: Challenge 2 ======

===== Clusters with a mass function =====


**PI**: Miklos Peuten\\
**Other participants**: Mark Gieles, Adriano Agnello, Alice Zocchi, Antonio Sollima, Vincent Henault-Brunet, Anna Lisa Varri

Questions to address: 

  - Can the mass segregation be reproduced by multi-mass King models? 
  - How important is the effect of mass segregation?
  - How correct is the assumption of energy equipartition?

Example of comparison between isotropic multi-mass model and N-body model with 100% retention fraction of stellar BHs:\\
{{:multi-mass.png}}

==== Effect of metallicity ====
Density and velocity profiles of clusters with different mass function:\\
{{:density-velocity-mm.png}}

Importance for mass-to-light ratio: (Shanahan et al. to be submitted):\\
{{:mass-to-light-m31.png}}

The relevant snapshots from simulations with a mass function are available in [[:tests:collision:mock_data|section B of the Mock data page]].

The definition of the stellar types (KSTAR) used in the ''NBODY6'' snapshots can be found in the [[:tests:collision:mock_data|Appendix section of the Mock data page]].


==== Anisotropy in multi-mass models ====

{{:multi-mass_michie_df.png}}

Anisotropy profile of different components in multi-mass clusters. Left: N-body simulation with 10% retention fraction of black holes. Right: Three-component multi-mass Michie model. 
{{:beta_multi-mass.png}}


Anisotropy profile of different mass components in Michie-King multi-mass model constructed with a dependence of the anisotropy radius on stellar mass.
{{:beta_multi-mass_eta.png}}


Anisotropy profile of different components in multi-mass cluster, N-body simulation with 100% retention fraction of black holes.
{{:beta0p5gyr.png}}