We present V,I light curves for 12 variable stars identified in the newly discovered satellite of the Milky Way in the Bo { \ddot { o } } tes constellation ( 2 ) .
Our sample includes 11 RR Lyrae stars ( 5 first overtone , 5 fundamental mode and 1 double mode pulsator ) , and one long period variable close to the galaxy red giant branch tip .
The RR Lyrae stars trace very well the average V luminosity of the galaxy horizontal branch , leading to a true distance modulus for the galaxy of \mu _ { 0 } =19.11 \pm 0.08 mag for an assumed metal abundance of [ Fe/H ] = -2.5 ( 20 ) , and for E ( B - V ) =0.02 mag .
Average periods are \langle Pab \rangle =0.69 d and \langle Pc \rangle =0.37 d for ab- and c- type RR Lyrae stars , respectively , making of Bo { \ddot { o } } tes the second pure Oosterhoff type II ( OoII ) dSph after Ursa Minor .
The location of the double mode RR Lyrae ( RRd ) in the Petersen diagram is consistent with RRd stars in OoII clusters , and corresponds to an intrinsic luminosity of logL / logL \odot =1.72 ( for Z=10 ^ { -4 } and M=0.80 M \odot ) according to Bono et al .
( 3 ) pulsation models .