Comparison of WISE W1/W2 and Spitzer ch1/ch2 photometry for mid–late T dwarfs, Y dwarfs, and T/Y subdwarf candidates. W2 and ch2 remain tightly correlated with effectively zero systematic offset across the range of M _W2 and J − W2 values spanned by this sample. On the other hand, there is considerable scatter between W1 and ch1 magnitudes, with this scatter becoming larger for increasing M _W2, W1, and J − W2. This suggests that caution ought to be exercised when attempting to select cold, low-metallicity candidates based on WISE W1 − W2 color only, as has been previously attempted/suggested in Meisner et al. (2021) and Brooks et al. (2022).