We present high-precision photometry of the hypervelocity star SDSS J090745.0+024507 ( HVS ) , which has a Galactic rest-frame radial velocity of v = 709 { ~ { } km s ^ { -1 } } , and so has likely been ejected from the supermassive black hole in the Galactic center . Our data were obtained on two nights using the MMT 6.5m telescope , and is supplemented by lower precision photometry obtained on four nights using the FLWO 1.2m telescope . The high-precision photometry indicates that the HVS is a short-period , low-amplitude variable , with period P = 0.2 - 2 { ~ { } days } and amplitude A = 2 - 10 \% . Together with the known effective temperature of T _ { eff } \simeq 10 , 500 ~ { } { K } ( spectral type B9 ) , this variability implies that the HVS is a member of the class of slowly pulsating B-type main sequence stars , thus resolving the previously-reported two-fold degeneracy in the luminosity and distance of the star . The HVS has a heliocentric distance of 71 ~ { } kpc , and an age of \lesssim 0.35 ~ { } { Gyr } . The time of ejection from the center of the Galaxy is \leq 100 Myr , and thus the existence of the OS constitutes observational evidence of a population of young stars in the proximity of the central supermassive black hole \sim 0.1 Gyr ago . It is possible that the HVS was a member of a binary that was tidally disrupted by the central black hole ; we discuss constraints on the properties of the companion ’ s orbit .