and we use the mean magnitudes from his observations, converting $V-I_K$ values to $V-I_{\rm c}$ using the transform in Bessell([@bessell79]). V2 and LW10 are missing because the stars were saturated or unmeasurable on some of our $I$ frames.

Figure\[cmd\] illustrates that all variables in our sample, with the possible exception of V19, are almost certainly on the upper giant branch of 47Tuc (rather than in the SMC or Galactic halo). V19 is located above and to the left of the 47Tuc AGB. There is no indication for a long secondary period in this star (see Fig.\[lctime\]) which may lead to a non-representative measurement[^1]. At the blue end of the giant branch where V19 is found, its amplitude of more than 0.8mag is rather untypical. Possible explanations may be that it has a very close blue neighbour that was not separated from V19 in our images, or it may be a star in the Galactic halo.

The most interesting aspect of Figure\[cmd\] is that it clearly shows that all stars on the giant branch of 47Tuc redder than $V-I_{\rm c}$$\approx$1.8 are variable.

Finally, we comment on the connection between LPV pulsation and mass loss in 47Tuc. Origlia et al.([@origlia02]) listed five 