# What is the local stellar number density?

Is it just me or does this paper, while providing a great equation for the behaviour of the general stellar number density, never actually give a value for the local stellar number density $$\rho(R={\rm R}_\odot, z=0)$$? I want to use their relationship for a calculation in my Master's thesis but I'm not sure what value for the local stellar density I should be using.

While some values (dimensionless, I assume number per light-year cubed) are present in figures 21 & 24 and tables 6 & 7 these are only for certain binned-by-colour stellar populations and not the general value. The value is conspicuously absent from table 10 which contains every other parameter. And it is not even addressed in equation 19 where it is introduced. Is there a particular reason for all this?

I hope I'm just missing something, and I could always use a rough value like the '$$0.004$$ stars per cubic light year' used by Erik Gregersen in 'The Milky Way and beyond' (The Rosen Publishing Group. pp. 35–36. ISBN 1-61530-053-8), but any inside insight would be appreciated.

As an aside, I am also assuming 'stellar number density' includes non-main-sequence stars, i.e. giants and white dwarfs. Is that correct?