a <mag> is the intensity mean over the cycle, Amp is the amplitude of a Fourier fit to the light curve, and s_<mag> is the rms scatter of the individual points about the Fourier fit. The period from Table5 was used unless flagged by footnote g in this table.
b The variation in the NSVS data was judged to be of marginal significance; see the text for a discussion. <mag> is the arithmetic mean of all the nightly mean magnitudes, and rms is the rms scatter about the mean magnitude. Amp is not listed.
c This star is a likely variable in the NSVS data but no meaningful period could be determined for the NSVS data, the variation was irregular or the phase coverage of the NSVS data was inadequate for a Fourier fit. <mag> is the arithmetic mean of the all the nightly mean magnitudes, and Amp is the difference between the medians of the five faintest and five brightest magnitudes. No rms is given.
d See a note for this star in Column N.
e One or a few anomalous magnitudes were deleted from the NSVS data before determining <mag>, Amp, and rms. 
f Also identified by Hoffman et al.  (2009, cat. J/AJ/138/466). 
g The NSVS period from Table6 was used.  
h There are two or more stars near the putative variable location on the sky. They are apparently blended in the NSVS photometry so <m> must be used with caution.
p Using the period from column (2), <Vmag> and <V-R> are the intensity means over the cycle, Vamp is the amplitude of a Fourier fit to the light curve, and s_<Vmag> is the rms scatter of the individual points about the Fourier fit.
q The variation in the Behlen data was judged to be of marginal significance. <Vmag> and <V-R> are the arithmetic means of the nightly mean magnitudes and colors, and s_<Vmag> is the rms scatter about the mean magnitude. Vamp is not listed.
r This star is a likely variable in the Behlen data but no meaningful period could be determined for the Behlen data, the variation was irregular or the phase coverage of the Behlen data was inadequate for a meaningful Fourier fit. <Vmag> and <V-R> are the arithmetic means of the nightly mean magnitudes and colors, and Amp is the range of the observed magnitudes. No rms is given.
s Based on the light and color curve this star is possibly an eclipsing binary.
t Variable amplitude. 
u Possibly the mean magnitude varies over hundreds of days based on variations within the NSVS data set or between the NSVS and Behlen data sets.
v No period or time scale satisfies all of the data. The best value for the Behlen data is tabulated.
i The shape of the light curve varies or there is phase jitter present.
j No period or time scale fits all of the data but there are too few data from Behlen to determine them. The overall best value is tabulated and was used in the analysis.
k No meaningful period or time scale was found for the Behlen photometry. The tabulated value was derived from the NSVS data only.
l Not used.    
m One or a few anomalous points were omitted from the analysis. 
n The standard error of the zero point of the magnitudes and/or colors for the comparison stars was between 0.015 and 0.050mag.
o The zero point of the magnitudes and/or colors of the comparison stars was uncertain by more than 0.05mag due to the availability of only a single photometric night for this field, poor agreement between two photometric nights, or unusual scatter in the magnitudes and/or colors. Hence, the values of the magnitudes and colors in columns <Vmag> and <V-R> are of questionable reliability.