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Table 1

Parameters used in the assumed galaxy model.

# Component   [M  pc-3] σz,i(0)   [km  s-1] σz,i(0)   [km  s-1] hi   [pc]
(observation) (observation) (MCMC) (MCMC)

1 H2 0.021 4.0 3.80 ± 1.0 32.4
2 HI(1) 0.016 7.0 7.00 ± 1.0 63.4
3 HI(2) 0.012 9.0 9.02 ± 1.0 84.7
4 Warm gas 0.0009 40.0 40.1 ± 2.0 564
5 Giants 0.0006 20.0 20.0 ± 2.0 224
6 Mv < 2.5 0.0031 7.5 7.56 ± 2.0 69.2
7 2.5 < Mv < 3.0 0.0015 10.5 10.7 ± 2.0 103
8 3.0 < Mv < 4.0 0.0020 14.0 14.1 ± 2.0 144
9 4.0 < Mv < 5.0 0.0022 18.0 18.1 ± 2.0 197
10 5.0 < Mv < 8.0 0.007 18.5 18.5 ± 2.0 203
11 Mv > 8.0 0.0135 18.5 18.4 ± 2.0 201
12 White dwarfs 0.006 20.0 20.1 ± 5.0 226
13 Brown dwarfs 0.002 20.0 20.0 ± 5.0 224
14 Thick disk 0.0035 37.0 37.7 ± 5.0 519
15 Stellar halo 0.0001 100.0 99.8 ± 10.0 1891

Notes.This model assumes the fifteen visible components shown in the second column, following Garbari et al., in which their disk mass model is taken from Flynn et al. (2006, the third and fourth columns). In this model, we adopt ρdm = 0.01  M  pc-3 and derive hi (the last column) with MCMC calculation. Using the set of hi, the fifth column is recalculated by Eq. (8). Our assumed model of Eq. (6) uses the third and sixth columns. The uncertainties on σz,i(0) are set to be the same as in Garbari et al..

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