see text; (5) current periodicity unclear, see Lebzelter et al. ([@LWHJF05]) for details; (6) close neighbour on 2MASS images, NIR fluxes and position possibly wrong; (7) not in 2MASS point source catalogue, coordinates calculated from our images, $K$ magnitude from Origlia et al. ([@origlia02]); (8) only on Mount Stromlo frames; (9) no Mount Stromlo data; (10) stars with near infrared excess detected by Origlia et al. ([@origlia02]); (11) see text in Section\[var\_section\] for comments on the periods. \[variables\]

Light variation versus time are presented in Figure\[lctime\], together with the fits from Fourier analysis. For selected variables with a reliable period determination and no long secondary period we show the light curve plotted against phase in Figure\[lcphase\]. In Fig.\[lctime\] obvious deviations of the data from the fit illustrate the semiregular nature of many stars of the sample. It can be seen that quite a large fraction of variables shows a long secondary period lasting several hundred to several thousand days. As these periods exceed the length of the time span monitored, we could not determine their length accurately and thus we do not give them in Table\[variables\]. They are included in the fits for illustrative purposes only. The formal ratio between 