We present high signal precision optical reflectance spectra of 2005 FY9 taken with the Red Channel Spectrograph and the 6.5-m MMT telescope on 2006 March 4 UT (5000-9500 Å; 6.33 Å pixel -1) and 2007 February 12 UT (6600-8500 Å; 1.93 Å pixel -1). From cross-correlation experiments between the 2006 March 4 spectrum and a pure CH 4-ice Hapke model, we find the CH 4-ice bands in the MMT spectrum are blueshifted by 3 ± 4 Å relative to bands in the pure CH 4-ice Hapke spectrum. The higher resolution MMT spectrum of 2007 February 12 UT enabled us to measure shifts of individual CH 4-ice bands. We find the 7296, 7862, and 7993 Å CH 4-ice bands are blueshifted by 4 ± 2, 4 ± 4, and 6 ± 5 Å. From four measurements we report here and one of our previously published measurements, we find the CH 4-ice bands are shifted by 4 ± 1 Å. This small shift is important because it suggest the presence of another ice component on the surface of 2005 FY9. Laboratory experiments show that CH 4-ice bands in spectra of CH 4 mixed with other ices are blueshifted relative to bands in spectra of pure CH 4-ice. A likely candidate for the other component is N 2-ice because its weak 2.15 μm band and blueshifted CH 4 bands are seen in spectra of Triton and Pluto. Assuming the shift is due to the presence of N 2, spectra taken on two consecutive nights show no difference in CH 4/N 2. In addition, we find no measurable difference in CH 4/N 2 at different depths into the surface of 2005 FY9.