Two Short-Period Eclipsing Binary Stars in the Field of PG 1047+003

We present extensive time-series photometry confirming that two stars located in the field of PG 1047 + 003 are short-period eclipsing binary systems. One of these stars, published as a photometric standard by Landolt and designated as PG 1047 + 003C, is shown to have eclipse depths on the order of 0.1 mag and a period of ∼0.28 days. The other star, located ∼2^‧ south-southwest of PG 1047 + 003, exhibits a similar amplitude and light-curve shape, but has a slightly longer period of ∼0.35 days. Light-curve solutions for both variables, based on the Wilson-Devinney code, reveal them to be contact binaries with low inclinations and each possessing uneven maxima, which we attribute to the presence of a single hot spot on the surfaces of the primary stars.