given as $\sigma_{cor}=1.33$. As the fitting is normalised, the error should also be normalised. Performing this normalisation results in a normalised standard deviation of $\hat{\sigma}_{cor}=0.028$. This values is set as the intensity error of the prominence, i.e. $\hat{\sigma}_{prom}=0.028$. It should be noted that this value is approximately the same as the standard deviation of the fluctuations shown in the prominence in Figure \[intfit\] for heights greater than $4$.

The fitting error is determined as the standard deviation of the difference between the normalised intensity and the fit at each pixel. These errors are shown in Table \[gam\_table\]. The error bars equivalent to $2\hat{\sigma}_{prom}$ and $2\hat{\sigma}_{fit}$ are shown in Figure \[intfit\]. The errors for ${M_*}^2$ from the fitting routine are also shown in Table \[gam\_table\].

![The graph shows a plot of intensity along the slit (solid line) and the fitting assuming the intensity proportional to density (dashed line) for $\gamma=1.65$. Error bars equivalent to twice the standard deviation are presented for the observed intensity and the fit.[]{data-label="intfit"}](figure11.eps){height="8cm"}

Using the value of $M_*$ from the fitting of the intensity and the definition of $M_*$ as: $$M_*=\sqrt{\frac{1}{D}}M_{\infty}=\sqrt{\frac{\gamma \beta_{\infty}}{\gamma \beta_{\infty}+2(\gamma-1)}}M_{\infty}$$ It is possible to solve for the plasma $\beta$ of the prominence, where $\beta$ 