Top: photometric monitoring of 51 Peg from Hipparcos, phase-folded on the orbital period of 51 Peg b. The x-axis is plotted such that transit would occur at phase = 0, respectively, if present in the light curve. Bottom: radial velocity curve for 51 Peg with our updated orbital solution (red solid line). The reduced ﹩{\chi }^{2}﹩ of the best-fitting model displayed here was 6.9, thus EXOFAST rescaled all of the RV uncertainties by a multiplicative factor of 2.6 to achieve ﹩{\chi }_{\nu }^{2}﹩ = 1 and counteract any underestimate of the RV uncertainties. The errors on the derived parameters in Table 2 reflect these increased RV uncertainties. The error bars in this plot have not been rescaled from the original literature values given in Table 1.