with the mass-to-light conversion $M_*/L_{R}$ for the stellar disc, we thus have four free parameters. We have considered using an additional mass-to-light conversion for the bulge, but found that with these four parameters the solutions were already becoming degenerate. Adding an additional free parameter would have worsened this problem.

We constrain $\rho_{0,\textrm{halo}}$ between 0 and 3 M$_\odot$ pc$^{-3}$, $R_c$ between 100pc and 10kpc, $q$ between 0.1 and 2.0, and $M_*/L_{R}$ between 0.5 and 3.0.

![image](Petersetal-Vfig1a.jpg){width="40.00000%"} ![image](Petersetal-Vfig1b.jpg){width="40.00000%"} ![image](Petersetal-Vfig1c.jpg){width="40.00000%"} ![image](Petersetal-Vfig1d.jpg){width="40.00000%"}

![image](Petersetal-Vfig2a.jpg){width="49.00000%"} ![image](Petersetal-Vfig2b.jpg){width="49.00000%"}

![image](Petersetal-Vfig3a.jpg){width="40.00000%"} ![image](Petersetal-Vfig3b.jpg){width="40.00000%"} ![image](Petersetal-Vfig3c.jpg){width="40.00000%"} ![image](Petersetal-Vfig3d.jpg){width="40.00000%"}

![image](Petersetal-Vfig4a.jpg){width="49.00000%"} ![image](Petersetal-Vfig4b.jpg){width="49.00000%"}

![image](Petersetal-Vfig5a.jpg){width="40.00000%"} ![image](Petersetal-Vfig5b.jpg){width="40.00000%"} ![image](Petersetal-Vfig5c.jpg){width="40.00000%"} ![image](Petersetal-Vfig5d.jpg){width="40.00000%"}

![image](Petersetal-Vfig6a.jpg){width="49.00000%"} ![image](Petersetal-Vfig6b.jpg){width="49.00000%"}

![image](Petersetal-Vfig7a.jpg){width="40.00000%"} ![image](Petersetal-Vfig7b.jpg){width="40.00000%"} ![image](Petersetal-Vfig7c.jpg){width="40.00000%"} ![image](Petersetal-Vfig7d.jpg){width="40.00000%"}

![image](Petersetal-Vfig8a.jpg){width="49.00000%"} ![image](Petersetal-Vfig8b.jpg){width="49.00000%"}

Results {#sec:hydrostaticresults}
=======

IC5249
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We have been moderately successful in modelling the dark matter halo of galaxy IC5249. The decomposition of both the optically thin and self-absorbing [ <span style="font-variant:small-caps;">HI</span> ]{} results is shown in Figure \[fig:IC5249decomposition\]. As is clear from the figure, the uncertainties in the stellar halo contribution, and subsequently the dark matter halo contribution are quite severe. This is mostly due to the fact that the measurements of both the vertical force gradient, as well as the rotation curve, start relatively far out (near 5.0-5.5kpc). The data of the inward parts of the galaxy were too uncertain for 