Hi Maze, i hope this helps, it was copied from Binney Tremaine, page 111,

(a) The Bulge the density of this components is assumed to be

ρb(R,z)=ρb0(m/ab)^(-alphab) exp{m^2/rb^2}

where

m = sqrt{R^2 + z^2/qb^2}

For qb < 1 this is an oblate, spheroidal power-law model that is truncated

at an outer radius rb.

Near-infrared photometry (BM x10.2.1) suggests values for three of the parameters,

alphab = 1.8, qb = 0.6, rb = 1.9 kpc, and without loss of generality, we can set ab = 1 kpc. The parameter ρb0, and hence the mass of the bulge, are determined by tting the dynamical constraints.

...

(c) The stellar disk The density of the stellar disk is assumed to fall o

exponentially with radius R, as in equation (1.7), and to depend on distance

from the midplane z through the sum of two exponentials, representing the

thin and thick disks described on page 13|this dependence on z is motivated

by observations such as those of Gilmore & Reid (1983), shown in BM Figure

10.25. Mathematically,

ρd(R, z) = Σd exp{-R/Rd}((α0/2z0) exp{-|z|/z0}+(α1/2z1) exp{-|z|/z1})

where α0 + α1 = 1, ∑d is the central surface density, Rd is the disk scale

length, and z0 = 0.3 kpc and z1 = 1 kpc are scale heights for the thin and

thick components.

sorry i cant help more than that but i was looking for the same stuff, its a shame no one uploaded a plot -observed- or at least smthn about the density profile [V] [V] [V]