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--- tests:collision:gc2_archive [2015/08/31 12:22] – v.henault-brunet
+++ tests:collision:gc2_archive [2022/10/24 12:26] (current) – external edit 127.0.0.1
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-===== Summary of GC2 Workshop =====
+===== GC II =====
 Summary from the Collisional Systems working group at the Gaia Challenge 2 workshop in Heidelberg (26-31st October 2014).
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 [[:tests:collision:gc2_archive:challenge1|Challenge 1]]: Zocchi et al. - The interplay between anisotropy and tides throughout the evolution of clusters. Comparison of f_nu and lowered isothermal models with and without (radial) anisotropy to N-body simulations of equal-mass clusters, isolated and within a tidal field.
-[[:tests:collision:challenge2|Challenge 2]]: Peuten et al. - Comparison of multi-mass models to N-body simulations with a full mass spectrum and different populations of dark remnants. Quantify the mass segregation parameter gamma (sigma_j ~ m_j^gamma) and anisotropy parameter eta (r_a  ~ m_j^eta).
+[[:tests:collision:gc2_archive:challenge2|Challenge 2]]: Peuten et al. - Comparison of multi-mass models to N-body simulations with a full mass spectrum and different populations of dark remnants. Quantify the mass segregation parameter gamma (sigma_j ~ m_j^gamma) and anisotropy parameter eta (r_a  ~ m_j^eta).
-[[:tests:collision:challenge3|Challenge 3]]: Sollima et al. - Biases in the determination of the masses and mass functions of clusters in different stages of evolution and different tidal fields. Comparison of lowered isothermal models (single-mass and multi-mass) to mock data from N-body simulations, mimicking real observations. Look at the effect of observing only RGB stars or RGB and bright MS stars, of having only LOS velocities or proper motions from Gaia, of missing kinematic data in the core, etc.
+[[:tests:collision:gc2_archive:challenge3|Challenge 3]]: Sollima et al. - Biases in the determination of the masses and mass functions of clusters in different stages of evolution and different tidal fields. Comparison of lowered isothermal models (single-mass and multi-mass) to mock data from N-body simulations, mimicking real observations. Look at the effect of observing only RGB stars or RGB and bright MS stars, of having only LOS velocities or proper motions from Gaia, of missing kinematic data in the core, etc.
 Alice, Miklos, and Antonio have taken the lead of the projects listed above. Everyone else is obviously welcome to contribute. If you’re name is not already listed in the wiki as an active participant of a project in which you would like to be involved, please let Vincent, Mark, and the PI of the project know what you want to contribute. We’ll then make sure you are included in future communications about this project.
-==== Additional challenges ====
-A few more ideas, still in the early stages, were discussed during the workshop:
-A. [[:tests:collision:challenge4|Challenge 4]]: Weighing dark remnants using luminous stars - Following discussions with Adriano, we decided to add another challenge in which we will explore how/if the mass function of dark remnants can be constrained from a limited set of observables, using mock data from N-body simulations. This could be part of Miklos’ project on Challenge 2. Provided that this works, we can then consider a direct application to real data (e.g. Gaia-ESO survey - some of us are members of the consortium).
-B. Mass modelling GCs with multiple populations - Pascal offered to apply his non-parametric method (developed for dwarf galaxies) to [[:tests:collision:new_challenges|mock data from an N-body simulation of a globular cluster with two distinct chemical populations]]. We want to get a feeling for how well the method recovers the mass distribution of a GC, and also how much do we gain by considering two tracer populations with different phase-space distributions.
-C. Dark remnants & IMBH - Laura is applying her discrete Jeans modelling method to snapshots of N-body models that contain stellar-mass black holes (from [[:tests:collision:challenge2|Challenge 2]]). The idea is check if a concentration of stellar-mass black holes near the centre can be mistaken for an intermediate-mass black hole. Anna S. has also been looking at the snapshots from Douglas Heggie’s M4 simulation, in particular at the potential kinematic signatures following the ejection of relatively massive black holes.
 ==== Progress report ====