My primary project concerned the Martian atmosphere. I analyzed, cataloged, and diagnosed data collected from the MAVEN orbiter's Imaging Ultraviolet Spectograph (IUVS) high resolution echelle channel.
This involves running a series of procedures incorporating spacecraft geometry, detector binning schemes, and other properties to plot the H and D Lyman-Alpha emission lines as seen above (the H
emission is the large peak you see, while the D emission is the very small spike just to the left of the H line). The x-axis represents the wavelength of the light in angstroms
and the y-axis represents the intensity of the emission line in photons/second.
I also searched through the mission to and classify how the background emission changed with respect to various feautres of spacecraft geometry.
THE REDUCTION EP