Lomb–Scargle periodograms (LSPs) of the activity indicators for each radial velocity (RV) data set (S-index for HIRES, FWHM for HARPS-N) show a notable peak at 6.5 days, which is one quarter the rotation period (or third harmonic of the rotation period) of the star. In the HIRES S-index LSP we identify a very tentative signal at 25 days (within one standard deviation of the rotation period of the star), while in the HARPS-N FWHM LSP there is not an identifiable signal at the rotation period. The strong peak at the third harmonic of the rotation period suggests that the rotation period of the star is consistent over the timescale of RV data collection and is consistent with the rotation period derived from the Kepler photometry.