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--- tests:collision:challenge3 [2014/10/23 13:47] – v.henault-brunet
+++ tests:collision:challenge3 [2015/08/31 12:37] (current) – removed v.henault-brunet
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-====== Challenge 3: Simulated observations and biases ======
-PI: Antonio Sollima\\
-Co-I: Alice Zocchi\\
-Other active participants: Mark Gieles, Vincent Henault-Brunet, ...
-Questions to address:
-  - How different are the fits when considering: 1) all stars and 2) only visible stars?
-  - Is it better to consider luminosity weighted profiles, or number density profiles?
-  - How much can we do with 2 velocity components instead of 1 (i.e. with Gaia data)?
-==== Dataset 1: Clusters in tidal fields with stellar evolution ====
-(Simulations ran and kindly made available by Holger Baumgardt)\\
-Here we consider 2 clusters which are slightly more realistic:
-  - IC: King (1966) W_0 = 5 model, N = 131072, Kroupa (2001) mass function between 0.1-15 Msun (no black-holes).
-  - No primordial binaries, no central black hole, circular orbit in logarithmic halo with V = 220 km/s.
-  - Z = 0.001
-  - Stellar evolution and mass-loss according to Hurley et al. (2000, 2002)
-  - 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.
-  - {{:data:W05_N131K_RG8.5_FEH-0.0_T10.gz}} UPDATED! Thursday August 22
-  - {{:data:W05_N131K_RG8.5_FEH-0.0_T100.gz}} UPDATED! Thursday August 22
-  - {{:data:W05_N131K_RG8.5_FEH-0.0_T1000.gz}} UPDATED! Thursday August 22
-  - {{:W05_N131K_RG8.5_FEH-0.0_T12000.gz}}
-  - {{:data:W05-N131K_RG15_FEH-0.0.T10.gz}} NEW! Tuesday August 20
-  - {{:data:W05-N131K_RG15_FEH-0.0.T100.gz}} NEW! Tuesday August 20
-  - {{:data:W05-N131K_RG15_FEH-0.0.T1000.gz}} NEW! Tuesday August 20
-  - {{:W05_N131K_RG15_FEH-0.0_T12000.gz}}
-==== Dataset 2: Snapshots of an N-body model of M4 ====
-As another source of mock data, snapshots from a large N-body simulation of the globular cluster M4 are [[http://datashare.is.ed.ac.uk/handle/10283/618?show=full| 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.