Bus et al. report: Below is a composite plot, showing the IRTF data, along with Moskovitz et al. data from the DCT taken the following night (the DCT visual-wavelength spectral plot was simply scaled to match the axes of the IRTF data, shifted vertically to match in the overlap region between 0.82 and 0.9 microns, and pasted on). A plot containing mean spectra for the Bus-DeMeo Xc and Xe classes is also overlaid. This overlay of plots was done as a quick test, but the results are interesting. There is no sign of a thermal tail out to 2.4 microns. Even though the formal error bars and scatter of the points in the K-band are large, a thermal signature if it were present should have been detected. Instead the flux at the red end of the spectrum just disappears into the sky noise, producing the large scatter. Comparison to other taxonomies shows that the Xc class is commonly associated with M-types, while the Xe class more commonly contains E types. The Xc and Xe classes are very similar in the near-IR, but diverge some in the visible portion of the spectrum with the biggest difference near 0.7 microns. Given the better match of the MAskovitz et al. spectrum to the Xc class around 0.7 microns. Bus indicates that 2012 TC4 is more likely to be an Xc (M-type) than an Xe (E-type).