  The Intergalactic Medium (IGM) contains $>$50% of the baryonic mass of the
Universe, yet the mechanisms responsible for keeping the IGM ionized has not
been fully explained. Hence, we investigate ion abundances from the largest
blind QSO absorption catalog for clouds that show C IV, N V, and O VI
simultaneously. The wavelength range of present UV spectrographs, however, make
it possible to probe C IV and O VI over a small range of redshift ($z \approx
0.12 - 0.15$). As a result, we only have five IGM absorbing clouds, yet these
provide a powerful and representative tool to probe the IGM ionization state.
We found one cloud to be in collisional ionization equilibrium while three of
five showed signs of being produced by non-equilibrium processes, specifically
conductive interfaces and turbulent mixing layers. None of the models we
explore here were able to reproduce the ionization state of the remaining
system. Energetic processes, such as galactic feedback from star formation and
AGN winds, would be excellent candidates that can cause such widespread
ionization.
