Galactic population repartition in the BGM1 biased simulations.
|Thin disc||Thick disc||Halo|
|LRa01 BGM1 age||96%||4%||0%|
|LRc01 BGM1 age||82%||17%||1%|
|SRc01 BGM1 age||95%||5%||0%|
|LRa01 BGM1 kine.||87.7%||2.6%||0.0%|
|LRc01 BGM1 kine.||76.0%||6.2%||0.5%|
|SRc01 BGM1 kine.||86.1%||3.6%||0.0%|
|LRa01 OBS. kine.||58%||18%||0.3%|
|LRc01 OBS. kine.||48%||20%||5%|
|SRc01 OBS. kine.||82%||2.4%||0.0%|
Notes. “age” or “kine” correspond to the method used to separate the stellar populations: “age” is related to the age flag returned by the BGM1 and “kine” denotes classifications based on the Bensby et al. (2005) method using velocity components. For the kinematical results, the sum of the three component does not reach 100% because it is a probabilistic way to disentangle the stellar populations, and some stars have intermediate kinematical parameters.
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