I've added an additional column to the data. Column 11 is a measurement of the "power" in the given spectral line. Here's a plot showing the MgII k and h power. The x-axis is the power and the y-axis is the number of vertical arcseconds from the center of the Sun.
The total power corresponds as expected to the shape of the spectral lines: less power where the spectrum is dark, more power where the spectrum is bright ---
|k (left) and h (right) MgII spectral lines|
Although now apparent when looking at the image, the plot of total power shows that the h lines are typically brighter than the k lines.