This star showed considerable surface activity; the rotation rates (or, more precisely, the frequency of probable-repeating star-spots) was 5.19 ± 0.04 days. Further, it appears that the transit or eclipse times are unrelated to stellar variability suggesting that, if it is an EB with no minor eclipses visible, it is of the "detached" type. Identical values for T_FWHM and tau were obtained for every transit (or eclipse) via EXOFAST evaluations, which is consistent with either an exoplanet's grazing transits or an EB's major eclipses. No evidence for corresponding minor eclipses (if this is an EB) was observed. In either case, no definitive evidence for a TTV was obtained; there was a hint of such, but errors were too large to allow confirmation via a Lomb-Scargle Periodogram.