fit the data, which did not result in a stable fit. Smoothing was applied on the input parameters, but this did not improve the quality of the observed vertical force gradient. As such, we hereby present our best fit, but encourage the reader to have a skeptical treatment of them.

The self-absorbing [ <span style="font-variant:small-caps;">HI</span> ]{}model of the galaxy results in a dark matter core density $\rho_0$ of $0.015^{+0.001}_{-0.001}$M$_\odot$/pc$^3$, a scale length $R_c$ of $3.02^{+0.03}_{-0.08}$kpc and an oblate shape of $q=0.5^{+0.1}_{-0.1}$. The stellar disk is found to have a high $M_*/L_R=2.89^{+0.11}_{-0.44}$. The optically thin [ <span style="font-variant:small-caps;">HI</span> ]{}model produces a more massive central core density $\rho_0=0.022^{+0.004}_{-0.001}$M$_\odot$/pc$^3$, a shorter scale length of $R_c=2.30^{+0.10}_{-0.15}$ and a less oblate halo shape $q=0.7^{+0.1}_{-0.1}$. We again find a high $M_*/L_R=2.84^{+0.16}_{-1.15}$\
The cross-correlation diagrams of the models are shown in Figure \[fig:ESO115-crosscorr\].

ESO138-G014 {#sec:DM138}
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Galaxy ESO138-G014 was initially hard to model, as the total observed vertical force gradient was already weaker than the contribution from the neutral hydrogen alone. As we noted before in Paper III, the galaxy seems to have quite a thick [ <span style="font-variant:small-caps;">HI</span> ]{}layer (see Figure 13 of Paper III). The most likely explanation for this is that the galaxy is 