  We make the first observation-based calculation of the energy that goes into
cosmic-ray protons versus cosmic ray electrons in shock acceleration during
structure formation. We find a ratio of energy in cosmic ray protons to energy
in cosmic ray electrons of 0.86. This value, calculated from the non-thermal
X-ray component reported here from RTXE and the Fermi LAT upper limit for
gamma-ray emission, is significantly lower than theoretical estimates that
place most of the non-thermal energy in protons. Our estimate is based on the
detection of non-thermal X-ray emission using the 3 - 20 keV RXTE spectrum,
which shows residual emission not well modeled by a single thermal component.
The statistical significance of adding a non-thermal, power law component is
~96%. The significance of adding a second thermal component is 90%. The
addition of a component consisting of full Cosmic X-ray Background (CXB)
fluctuation to an isothermal model is significant with 92% confidence. The
cumulative probability for the two thermal component model is 81% and 90% for
the thermal plus power law. Thus the model with non-thermal emission is the
preferred description of the data. Evidence of shock heating between the
clusters in the spectro-imaging data of XMM, Chandra, and Suzaku indicates that
a cosmic ray component should also be present and supports a non-thermal
interpretation for the additional component. The bolometric non-thermal X-ray
luminosity is 1.6$\times$10$^{44}$ ergs s$^{-1}$, 36% of the total X-ray
emission in the 0.1 - 100 keV band.
