found 31 sources which showed a modulation in their lightcurve on a period between 51–83 mins and had a mean brightness of $g=15.9-20.8$. The full-amplitude of the modulation is in the range 0.05–0.65. We show their photometric properties in Table \[candidates\] and the light curves in Figure \[curves1\] and \[curves2\].

Distances {#distance}
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There is a clear relationship between $M_{V}$ and pulsation period which is applicable to SX Phe, $\delta$ Sct and RR Lyr stars (eg McNamara 1997). This Period-Luminosity (PL) relationship is consistent with a study of different types of short period pulsators in the Fornax dwarf spheroidal galaxy (Poretti et al 2008). Since the PL relationship of McNamara (1997) is calibrated with respect to $M_{V}$, we applied a small correction to transform our $g$ band magnitudes to that of the $V$ band (Jester et al 2005). Further, we used a NASA/IPAC tool[^1] which uses the maps of Schlegel, Finkbeiner & Davis (1998) to determine extinction to the edge of the Galaxy.

The PL relationship assumes that the period is the fundamental radial pulsation mode rather than the first over-tone which can also be observed in these stars. Given the short duration of our light curves, it is difficult 