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Table 5

Most important ingredients of the old and new model, which have been analysed.

Ingredients Old model New default models
model A model B

IMF Haywood-Robin Haywood-Robin (A) Kroupa-Haywood v6 (B)
SFR constant a decreasing exp( − 0.12τ) a decreasing exp( − 0.12τ)
Aumer & Binney (2009) Aumer & Binney (2009)
evolutionary see Table 2 package E2 Table 2 package E2 Table 2
tracks
age–metallicity Twarog (1980) Haywood (2006) Haywood (2006)
relation
atmosphere BaSeL 2.2 BaSeL 3.1 BaSeL 3.1
models
binarity no yes: from Arenou (2011) yes: from Arenou (2011)
thin disc age 10 Gyr 10 Gyr 10 Gyr
thick disc xl = 400 pc, hz = 800 pc xl = 400 pc, hz = 800 pc xl = 400 pc, hz = 800 pc
parameters density = 0.0083 */pc3 density = 0.0083 */pc3 density = 0.0083 */pc3
extinction Drimmel & Spergel (2001) Drimmel & Spergel (2001) Drimmel & Spergel (2001)
model + Marshall et al. (2006) + Marshall et al. (2006)
ISM local Robin et al. (2003) Binney & Tremaine (2008) Binney & Tremaine (2008)
density
local stellar Wielen (1974) Wielen (1974) Jahreiß & Wielen (1997)
mass density
age–velocity Gómez et al. (1997) Gómez et al. (1997) Gómez et al. (1997)
relation
warp Reylé et al. (2009) Reylé et al. (2009) Reylé et al. (2009)
scale length young disc hR = 5000.0 pc young disc hR = 5000.0 pc young disc hR = 5000.0 pc
old disc hR = 2400.0 pc old disc hR = 2400.0 pc old disc hR = 2400.0 pc

Notes. Notice that the two default models differ only by the IMF and the value of the local stellar mass density. The Drimmel & Spergel (2001) extinction model was not used in the BGM from Robin et al. (2003), but it was used here in the old model simulations.

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