the emission is scattering dominate ($\propto \rho$). In this paper we do not take into account the change in emission from the change in temperature. The fitting for the density is shown by the dotted line. This fit is performed using the IDL routine curvefit.pro. The fit solves for the value of ${M_*}^2$ giving the values shown in Table \[gam\_table\].

It is important to determine the error associated with this fit, so that the error in the plasma $\beta$ can later be calculated. There are two important errors that are associated with this fit: the intensity error and the error between the observed curve and the model curve. These errors then determine the error for ${M_*}^2$.

The intensity error is determined in a simple fashion. The fluctuations of intensity in the corona above the prominence are used. Here we assume that the fluctuations in the Ca II H line (which should not have a coronal signal) are due to stray light, and so we assume this is representative of the error in the intensity. For a region in the corona above the prominence of size \[200,100\] pixel taken over 100 consecutive frames, the standard deviation of the intensity fluctuations is 