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--- tests:collision:mock_data:challenge_4 [2017/03/06 11:54] – v.henault-brunet
+++ tests:collision:mock_data:challenge_4 [2022/10/24 12:28] (current) – external edit 127.0.0.1
@@ Line 4: / Line 4: @@
-The mock data is a snapshots of 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 [[http://arxiv.org/abs/1409.5597]], which should be cited when making use of this data.
+The mock data is a snapshots of 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 this paper [[http://arxiv.org/abs/1409.5597]], which should be cited when making use of this data.
-We selected the snapshot at t = 12023.9 Myr and assume that radial/LOS velocities are available for all stars brighter than V=15 (N=1143). A distance modulus of 11.35 mag was adopted (i.e. D=1862.1 pc). The cluster properties are:
+We selected the snapshot at t = 12023.9 Myr. A distance modulus of 11.35 mag was adopted (i.e. D=1862.1 pc). The cluster properties are:
-  - M = 69144.5 M_sun
+  - Mtot = 69144.5 M_sun
   - L_V = 35547.1 L_V_sun
-  - M/L_V=1.95
+  - M/L_V = 1.95 Msun/L_V_sun
+  - <m> = 0.495 Msun
   - r_h = 3.14 pc
+  - r_eff = 1.43 pc
+  - N neutron stars = 130
+  - N black holes = 2
+  - Mass in remnants = 27176.4 Msun
 We do the comparison in 3 steps:
-  - Surface brightness profile + RVs
+  - Step 1: Surface brightness profile + RVs
-  - Surface brightness profile + RVs + PMs
+  - Step 2: Surface brightness profile + RVs + PMs ('HST')
-  - Surface brightness profile + RVs + PMs + Gaia
+  - Step 3: Surface brightness profile + RVs + PMs ('HST' + 'Gaia')
+(+ local mass function for methods allowing it).
-The data for the 3 fitting steps :
-  - Step 1:
-    - Surface brightness: {{:data:M4_sb.dat.gz}}
-    - Discrete LOS velocities: {{:data:M4_rv.dat.gz}}
-    - LOS velocity dispersion profile: {{:data:M4_rv_disp.dat.gz}}
-  - Step 2:
-    - Discrete proper motions: {{:data:M4_pm_mock.dat.gz}}
-    - Proper motion dispersion profiles: {{:data:M4_pm_disp_mock.dat.gz}}
-  - Step 3:
-    - Gaia proper motions:
-    - Gaia proper motion dispersion profiles:
-For methods that allow it, you can also use constraints from a mock observed mass function at a projected radius of 300 arcseconds from the centre: {{:tests:collision:M4_mass_function.tab.gz}}
+** DOWNLOAD NEW M4 MOCK DATA (updated 21/03/2017)**: All the mock data you will need (and more!) are available and bundled [[https://www.dropbox.com/s/8kish5scgry2nbh/M4_mocks.tar.gz?dl=0|here]]. You can find a summary of the list of files in 'ReadMe_M4_mocks'.
-A number density profile for stars brighter than the main-sequence turnoff (V < 17 mag; corresponding to a turnoff mass of 0.82 solar masses) is also available ({{:tests:collision:M4_number_density.dat.gz}}). This can be used as an alternative/complement to the surface brightness profile.
+Included are the surface brightness profile, line-of-sight dispersion profile and discrete velocities for RGB stars, HST-like PM dispersion profiles and discrete velocities, Gaia-like (end-of-mission) PM dispersion profiles and discrete velocities (for M4, bulge and halo-like backgrounds), number density profile for bright stars, and local mass function. Mass profiles and the M/L_V profiles (in projection and 3d) are also available. Predictions from best-fit models should be compared to the 3d M/L_V profile.
-The mass profile in projection and the $M/L_V$ ratio in projection can be found here:
-  - {{:data:m4_Sigma.dat.gz}}