Section \[sec:MLdiscussion\], the most likely $M_*/L_R$ values lie close to 0.5. If we thus limit ourselves to the data points at $M_*/L_R<0.55$, we find for the optically thin [ <span style="font-variant:small-caps;">HI</span> ]{}an oblate halo with $q =0.76_{-0.03}^{+0.04}$. The core density of the dark matter halo is $\rho_0 = 0.017_{-0.001}^{+0.001}$M$_\odot$/pc$^3$ and its scale length is $R_c = 4.49_{-0.05}^{+0.02}$kpc. The self-absorbing [ <span style="font-variant:small-caps;">HI</span> ]{}model returns an even more oblate halo, with a shape of $q =0.55_{-0.03}^{+0.14}$, a core density of $\rho_0 = 0.014_{-0.003}^{+0.003}$M$_\odot$/pc$^3$ and a scale length of $h_0 = 5.19_{-1.01}^{+1.30}$kpc. Comparing the two models, we see that the dark matter halo of the self-absorbing [ <span style="font-variant:small-caps;">HI</span> ]{}requires a more oblate halo, with longer scale length $R_c$ and less massive central density $\rho_0$.

ESO115-G021
-----------

We have not been very successful in modelling ESO115-G021. As can be seen from the results in Figure \[fig:ESO115decomposition\], the observed vertical force gradient has a nearly flat slope near the inner parts of the galaxy ($R<4$kpc). This is problematic to fit to, as we always expect the vertical force gradient to get increasingly strong near the inner parts. We have attempted fitting only beyond $R=3.5$kpc, but this left only 2kpc in which we could 