dispersion for IC5249 and ESO138-G014. For UGC7321 the velocity dispersion drops from 10 [[km s$^{-1}$]{}]{}in the central parts to 8 [[km s$^{-1}$]{}]{}at 8 kpc, then remains constant at this level out to 10 kpc, after wich it increases to 12 [[km s$^{-1}$]{}]{}at 14 kpc. We have sufficient confidence in it to adopt it in our analysis.

Galaxy UGC7321 has a total B-band magnitude of 13.75 and V-band magnitude of 13.19 [@Taylor2005], giving a B-V band difference of 0.56.\[sec:estimateML\] To estimate the stellar mass to light ($M_*/L_R$) ratio, we use the model interpolation engine[^2], which is based on the @Worthey1994A and @Bertelli1994A stellar population models. Using a single burst, Salpeter (slope -2.35) IMF we find a good fit using a single population of 950Myr and \[Fe/H\]=0.0, with B-V=0.554. This would place $M_*/L_R$ in the Rc-band at 0.55. We have repeated this exercise for our other galaxies, each time finding $M_*/L_R\approx0.5$. We therefore adopt a mass to light $M_*/L_{R}=0.5$ as a lower boundary to the stellar disc mass, and use the reported R-band total luminosities reported in Table 3 of Paper IV. As an upper boundary, we adopt $M_*/L_{R}<3$. At solar metallicity, this would imply a single stellar population of approximately 8Myr. 