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GC III
Goals/projects for GC III workshop
A. Method comparison (a.k.a. Challenge #4):
For this Challenge, initiated in GC III in Barcelona, we decided to compare fitting methods
- Jeans modelling (Laura)
- Single mass DF modelling (Alice)
- Multimass DF modelling (Miklos)
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 the http://arxiv.org/abs/1409.5597, which should be cited when making use of this data. Jeans modelling vs. Distribution-function based models for fitting mock data of GCs. We will start with $N$-body snapshots of the M4 models by Heggie (2014): http://datashare.is.ed.ac.uk/handle/10283/618
B. Understanding Gaia errors:
What will Gaia actually give us (for GCs, open clusters, runaway stars, hypervelocity stars)? What can we do with TGAS?
C. Potential escapers:
a) quantify biases from ignoring them
b) towards self-consistent mixture models with potential escapers
D. Rotation:
include prescription for rotation in multi-mass DF models.