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tokens: which the sample was selected, i.e., all objects with significant C iv BLR size measurements. For five of the six Seyfert AGNs in Table 6 there are BH mass estimates from H β RM. In Table 7 we list these BH mass estimates as given in the database of Bentz Katz ( 2015 ). 14 14 http://www.astro.gsu.edu/AGNmass/ From a comparison of these mass estimates to our estimates from the C iv line in Table 6 , we find that for NGC 7469 and 3C 390.3, the BH mass estimates from the two lines are within the 1 σ uncertainties (i.e., the 1 σ uncertainties overlap). For NGC 3783 and NGC 4151, the BH mass estimates are within the 1.5 σ uncertainties (if we add the σ from both measurements), and for NGC 5548, they are within 2 σ . This resemblance in the mass estimates for the two emission lines increases the confidence in these results and in the ability of the RM method to give consistent mass estimates. Table 7 Black Hole Mass Estimates from H β Reverberation Mapping Note. Measurements from the database of Bentz Katz ( 2015 ) in units of . Note that the front page of the database lists the averaged mass measurements from all lines, and here we list the mass measurements from the H β line alone. 5. Summary We have reported the final results from a 13 yr spectrophotometric RM campaign on high-luminosity quasars. The spectrophotometric observations were supplemented by 18 yr of photometric monitoring, which improved the cadence and the accuracy of the spectrophotometric continuum light curves by adding to them the photometric light curves. All 11 objects with photometric light curves display continuum variability of 10%–70% over about six years in the rest frame. This value is similar to that reported in Paper I with data over a period that was about one-third of the current one. Six of the 11 objects were monitored spectroscopically. We identified C iv emission-line time lags for 3 objects, indicating C iv emission-line region sizes of about 100 to 250 light days. Together with data from previous studies, we have constructed a C iv BLR size–UV luminosity relation over eight orders of magnitude in UV luminosity; the slope of 0.45 ± 0.04 is consistent with previous studies and with photoionization theory. Although all our monitored AGNs show significant continuum variation, only in about half of them did we measure C iv time lag (the same fraction was also was found by Lira et al. 2018 ). This may indicate that the ionizing continuum behaves differently from the 1350 Å continuum we measured in this study. Although C iv is not a preferred line for the central BH mass determination, we derive the mass for the 19 objects with proper C iv RM data. We find that the mass scales approximately as the square root of the UV luminosity, but with a large scatter. The scatter probably results at least partly from the drawbacks of the C iv line for BH mass measurement, but probably also includes an intrinsic scatter in that relation for AGNs, e.g., different velocities for