We present results from a well studied \delta Scuti star discovered in the Large Magellanic Cloud ( LMC ) .
The absolute magnitude of the variable was determined from the Period-Luminosity ( P - L ) relation for Galactic \delta Scuti stars and from the theoretical modeling of the observed B,V,I light curves with nonlinear pulsation models .
The two methods give distance moduli for the LMC of 18.46 \pm 0.19 and 18.48 \pm 0.15 , respectively , for a consistent value of the stellar reddening of E ( B - V ) =0.08 \pm 0.02 .

We have also analyzed 24 \delta Scuti candidates discovered in the OGLE II survey of the LMC , and 7 variables identified in the open cluster LW 55 and in the galaxy disk by Kaluzny et al .
( 2003 , 2006 ) .
We find that the LMC \delta Scuti stars define a P - L relation whose slope is very similar to that defined by the Galactic \delta Scuti variables , and yield a distance modulus for the LMC of 18.50 \pm 0.22 mag .
We compare the results obtained from the \delta Scuti variables with those derived from the LMC RR Lyrae stars and Cepheids .
The corresponding distance moduli are : \delta Scuti stars 18.48 \pm 0.02 mag ( standard deviation of the weighted average of the three above solutions ) ; RR Lyrae stars 18.49 \pm 0.06 mag ; and Cepheids 18.53 \pm 0.02 mag .
We have assumed an average color excess of E ( B - V ) = 0.08 mag \pm 0.02 for both \delta Scuti stars and Cepheids .
Within the observational uncertainties , the three groups of pulsating stars yield very similar distance moduli .
These moduli are all consistent with the “ long ” astronomical distance scale for the Large Magellanic Cloud .