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We make the first observation-based calculation of the energy that goes intocosmic-ray protons versus cosmic ray electrons in shock acceleration duringstructure formation. We find a ratio of energy in cosmic ray protons to energyin cosmic ray electrons of 0.86. This value, calculated from the non-thermalX-ray component reported here from RTXE and the Fermi LAT upper limit forgamma-ray emission, is significantly lower than theoretical estimates thatplace most of the non-thermal energy in protons. Our estimate is based on thedetection 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%. Theaddition of a component consisting of full Cosmic X-ray Background (CXB)fluctuation to an isothermal model is significant with 92% confidence. Thecumulative probability for the two thermal component model is 81% and 90% forthe thermal plus power law. Thus the model with non-thermal emission is thepreferred description of the data. Evidence of shock heating between theclusters in the spectro-imaging data of XMM, Chandra, and Suzaku indicates thata cosmic ray component should also be present and supports a non-thermalinterpretation for the additional component. The bolometric non-thermal X-rayluminosity is 1.6$\times$10$^{44}$ ergs s$^{-1}$, 36% of the total X-rayemission in the 0.1 - 100 keV band.

RXTE Observation of the Non-thermal Emission from the Early Stage Merger in Abell 1750