large number of LPVs now known in 47 Tuc, we are now in a position to examine the PL relations in the cluster. We do this in the form of the $K$-$\log P$ relation, which is shown in Figure\[klp\_obs\]. Generally, we do not have $K$ light curves for the LPVs in 47 Tuc so we can not readily calculate mean $K$ magnitudes. However, a small number of the variables have been observed many times (see Fox [@fox82], Menzies & Whitelock [@mw85] and Frogel, Persson & Cohen [@fpc81]) and good estimates of the mean $K$ magnitude and $K$ amplitude can be obtained. For each star plotted on Figure\[klp\_obs\], the $K$ magnitude is the mean of the maximum and minimum observed $K$ magnitude. For stars without multiple observations, the 2MASS $K$ magnitude has been used. All $J$ and $K$ magnitudes have been converted to the AAO system using the conversions in Allen & Cragg ([@ac83]) and Carpenter ([@car01]): these are the values shown in Table \[variables\]. A comparison of the $K$ amplitude with the $V$ light amplitude obtained in the present study shows that the $K$ amplitude is approximately 20% of the $V$ amplitude. The error bars in Figure\[klp\_obs\] have a full 