length of 20% of the full visual amplitude of the pulsation mode associated with each point. Hence, they should represent the $K$ amplitude of the variables.

Also shown in Figure\[klp\_obs\] are the sequences of LPVs in the LMC as given by Ita et al. ([@ita04]). The magnitudes have been adjusted to bring them from an LMC distance modulus of 18.55 to a 47Tuc distance modulus of 13.50. The large-amplitude Mira variables fall close to sequence C, while the bulk of the smaller amplitude variables fall near, but not necessarily on, sequences B$^{+}$, B$^{-}$ and C$^{\prime}$. The lack of variables on sequences A$^{+}$ and A$^{-}$ may be real or it may be that these stars have amplitudes that are below our detection limit of $\sim$0.1 mag.

It is notable in Figure\[klp\_obs\] that the 47Tuc LPVs do not appear to fall exactly on the LMC sequences. For example, the majority of the smaller amplitude variables brighter than $K$=7 fall between sequences B$^{+}$ and C$^{\prime}$ while fainter than $K$=7, most variables fall between sequences A$^{-}$ and B$^{-}$ with a small number appearing to fall on sequence C$^{\prime}$. This is probably a result of the different masses of the stars in the 47Tuc and 