[ <span style="font-variant:small-caps;">HI</span> ]{}model finds a halo with a higher core density of $\rho_{0,\textrm{halo}} = 0.620^{+0.009}_{-0.007}$M$_\odot$/pc$^3$ and a scale-length of $R_c  = 0.41_{-0.01}^{+0.02}$kpc. Again, the optimal solution favors a prolate halo at $q =1.9^{+0.1}_{-0.3}$. In this case the mass-to-light is $M_*/L_{R}= 0.69^{+0.04}_{-0.06}$.

ESO274-G001
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Galaxy ESO274-G001 is one of the two galaxies from Paper III for which we could accurately measure the velocity dispersion. We model the galaxy in the standard way, setting the $M_*/L_{R}$ lower boundary at 0.5. Both the rotation curve and vertical force decomposition are shown in Figure \[fig:ESO274decomposition\], where we show the results for both the optically thin and self-absorbing [ <span style="font-variant:small-caps;">HI</span> ]{}models. Both models have reproduced the rotation curve and the vertical force gradient reasonably well, although the self-absorbing model was more successful at the vertical force gradient.

We show the cross-correlation diagram for the optically thin [ <span style="font-variant:small-caps;">HI</span> ]{}model in Figure \[fig:ESO274-crosscorr\] (left). There is a clear correlation between the various parameters, which is mostly due to the uncertainty in $M_*/L_{R}= 0.96^{+0.46}_{-0.42}$. The halo is oblate with $q =0.7^{+0.1}_{-0.1}$, $\rho_{0,\textrm{halo}} = 0.150^{+0.020}_{-0.022}$M$_\odot$/pc$^3$ and $R_c = 1.10^{+0.04}_{-0.03}$kpc. The mass to light ratio $M_*/L_{R}$ was $0.96^{+0.46}_{-0.42}$.

The cross-correlation diagram of the [ <span style="font-variant:small-caps;">HI</span> 