a reliable measurement of the tracers. As the dark matter halo shape $q$ can most accurately be constrained from the vertical force gradient in the inner parts of the galaxy [see @OBrien2010D], this lack of data does not allow us to constrain $q$ significantly. The optically thin [ <span style="font-variant:small-caps;">HI</span> ]{}model yields $q=1.5^{+0.5}_{-0.5}$, while the self-absorbing [ <span style="font-variant:small-caps;">HI</span> ]{}yields $q=1.0^{+0.4}_{-0.3}$.

The lack of a significant constraint on $q$ leads to strong correlations between the other parameters. This is reflected in the cross-correlation diagrams for the parameters, seen in Figure \[fig:IC5249-crosscorr\] (left) for the optically thin case, and Figure \[fig:IC5249-crosscorr\] (right) for the self-absorbing [ <span style="font-variant:small-caps;">HI</span> ]{}case. An oblate dark matter halo shape ($q<1$) produces a less massive stellar disc, with a shorter dark matter halo scale length $R_c$ and higher dark matter halo core density $\rho_0$. This behavior holds in both models. Over the whole dataset, we find that for an optically thin [ <span style="font-variant:small-caps;">HI</span> ]{}model the halo is found at $\rho_0 =0.007^{+0.005}_{-0.001}$M$_\odot$/pc$^3$, $R_c=5.45^{+0.21}_{-0.52}$kpc. The stellar disc is found with $M_*/L_R=2.62^{+0.38}_{-1.19}$. The self-absorption [ <span style="font-variant:small-caps;">HI</span> ]{}models return $\rho_0 = 0.004^{+0.003}_{-0.001}$M$_\odot$/pc$^3$, a scale length $R_c$ of $9.79^{+0.21}_{-2.06}$, and a stellar disc with $M_*/L_R=2.98^{+0.02}_{-1.17}$.

As we discussed in 