Table 1
Spatial, velocity, and luminosity distributions used in the current model.
| Model | Distribution | Distribution |
| variable | type | parameters |
|
|
||
| Galactic | Radial decay and | hr = 2.44 kpc (1) |
| plane (X,Y) | Monte Carlo rejection | σd = 0.35 kpc (1) |
|
|
||
| Vertical | Gaussian | μz = 0 kpc |
| position (Z) (2) | σz = 25 pc | |
|
|
||
| Radial | Gaussian | μr = 0 km s-1 |
| velocity (U) | σr = 5 km s-1 | |
|
|
||
| Tangential | Gaussian | μt = Θ0 = 240 km s-1 (1) |
| velocity (V) | σt = 9 km s-1 | |
|
|
||
| Vertical | Gaussian | μv = 0 km s-1 |
| velocity (W) | σv = 5 km s-1 | |
|
|
||
| Luminosity | Power | Cutoffs: 10-8L⊙, 10-3L⊙ |
| function (L) (3) | law | and α = −1.43 |
Notes. We assumed the sun’s vertical position to be z = 0 pc and any change in this value, which Goodman et al. (2014) suggested to be 25 pc, was found negligible at these scales.
Reference. (1) Reid et al. (2014); (2) Green & McClure-Griffiths (2011); and (3) Pestalozzi et al. (2007). Radial, tangential and vertical velocity dispersion values are discussed in Sect. 2.3.
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