We report on our efforts to use the data from 1E 0102.2-7219 to verify the low energy response model for the eROSITA CCDs. 1E 0102.2-7219 (hereafter E0102) is the X-ray brightest supernova remnant (SNR) in the Small Magellanic Cloud (SMC). E0102 has a line-rich spectrum that is dominated by emission from O, Ne, and Mg with very little or no Fe emission. The lack of Fe L shell emission makes E0102's spectrum particularly useful for the calibration of CCD-resolution instruments because line blending is minimized. The E0102 spectrum has been well-characterized by the RGS on XMM-Newton and the HETG on the Chandra X-ray Observatory. A standard spectral model has been developed by the International Astronomical Consortium for High Energy Calibration (IACHEC) and has been used by the current generation of X-ray instruments to improve their calibrations. We apply this model to the eROSITA data to investigate the gain, spectral redistribution function, and the detection efficiency. We compare the line fluxes for the OVII triplet, OVIII Ly-alpha, NeIX triplet, and the Ne X Ly-alpha line complexes to the current generation of instruments to determine the consistency of the absolute effective areas of the instruments at these energies.