A273 The photometric parameters for this star were taken from Schmidt et al. (2009, cat. J/AJ/137/4598; Paper II).
A277 The photometric parameters for this star were taken from Schmidt et al. (2009, cat. J/AJ/137/4598; Paper II).
B001 The scatter for the NSVS data refers to the flat maximum with observations during eclipse removed.
B004 There appears to be a short period of about 30d and a longer period of the order of several hundred days.
B014 Between the NSVS and the Behlen observations this star brightened by about 0.5mag and the period changed from 24.5d to 1.2437d.
B017 This star went through one maximum and two minima during the NSVS observations. The minima differ by ~0.2mag suggesting a double wave. The interval between the minima of 170days was used to analyze the NSVS observations.
B022 The NSVS data exhibits a double wave with alternating deep and shallow minima over the 182.6 day cycle. By the time of the Behlen observations one maximum has disappeared and there is a single maximum and minimum per cycle.
B027 A period of 54.805d is also possible.
B028 There is an apparent eclipse superimposed on a pulsational variation. The tabulated values were determined with data during eclipse removed. The period determined from the eclipse alone is 5.7269+/-0.0002d and the depth of the eclipse is approximately 0.35mag.
B029 This star brightened by about 0.3mag between the NSVS and Behlen observations and the amplitude diminished by about a factor of 4.
B030 During the first season of the Behlen observations, 9 observations between JD=2454768 and 2455092, this star varied with the same period and similar amplitude to those of the NSVS observations. In the second and third seasons, 12 observations between HD=2455433 and HD=2455984, no variation was observed larger than {+/-}0.05mag. The photometric parameters in Table5 refer to the first season while for the second season <Vmag> =14.09, <V-R> =0.64, and {sigma}_V_=0.029.
B031 Both the NSVS and the Behlen data exhibit a double wave with two approximately equal minima and two unequal maxima.
B036 Due to irregular behavior no reliable estimate of the color can be made at the time of the spectrum. No color excess is given.
B040 Irregular variation in the NSVS photometry except for a dip in brightness of 0.3mag between JD=2451473 and JD=2451499. Small variation during the Behlen observations is consistent with the NSVS behavior outside of the dip.
B041 Considerable scatter in the light curve suggests the presence of the Blazhko effect.
B042 Several low points in both Behlen and NSVS photometry may indicate the presence of narrow eclipses. A period of about 28.9 gives a small amplitude light curve in the Behlen data and fits the NSVS data reasonably well in view of the faintness of this star. It should be regarded as a suspected variable until further until the variation is further confirmed.
B043 The NSVS light curve resembles an eclipsing binary if the period is doubled. However, color changes do not support this interpretation.
B044 This star appears to have faded about 0.4mag between the NSVS and the Behlen observations and the variation ceased. A faint nearby star appears to be too faint to account for this behavior so we regard this as a suspected variable.
B046 The Behlen observations were spread over four observing seasons. Only during the second, JD=2454707 to 2454869 did the star exhibit regular variation. The tabulated period was determined from that season and the NSVS data and the photometric parameters are for that season. The mean magnitude of this star brightened between the NSVS and the Behlen observations.
B048 The only comparison star in the field was also variable. The data from eight photometric nights were used without the benefit of a comparison star.
B051 Although there is a fainter star about 45" from the putative variable, the variation in the NSVS data appears to be real. This star is retained as a suspected variable. Assuming that the companion has a negligible effect on the NSVS photometry, by the time of the Behlen observations the star had faded by about 0.4mag and had ceased variation.
B057 An eclipse approximately 0.15 cycles wide and 0.7mag deep is evident in the NSVS light curve. Although only one point from the Behlen photometry falls within the eclipse, it agrees well with the NSVS data indicating a stable period over time. Outside of eclipse there is a stable variation with the same period as the eclipses. The photometric parameters in Tables 1 and 5 were determined with observations during the eclipse removed. Including all the NSVS observations gives <mag> =12.06 and {Delta}m=0.948mag.
B073 The magnitude and scatter tabulated for the NSVS are based on data from JD=2551598 to 2551633. During the previous season, JD=2551460 to 2551497, the values were <mag> =14.62 and {sigma}_m_=0.16. By the time of the Behlen photometry the magnitude was still close to the later NSVS value and did not vary over the four years of Behlen coverage. While this star is possibly variable on a time scale of months or years it is most likely constant.
B074 A variation of the order of one magnitude over a period of hundreds of days is consistent with all of the data.
B079 A second maximum appears to come and go. The period refers to the interval between occurrences of the apparently stable maximum.
B080 A period of 0.53594d, a one day alias of the adopted period, is of nearly equal significance. The color is consistent with either a BL Her or an RR Lyr star but the large scatter suggests the presence of the Blazhko effect. Further photometry is needed to confirm the status of this star.
B085 At the tabulated period there is possibly a second minimum. The color variation suggests that this star is an eclipsing binary.
B090 This star exhibits a deep, 0.75mag, minimum in both the Behlen and NSVS data that could be an eclipse. This is supported by the presence of a second shallow minimum,  0.25mag, when the period is doubled. However, the color variation and the considerable variation away from minimum do not support this interpretation. Here we will regard this star as a semi-regular pulsator.
B105 There are multiple aliases of similar significance between 1.665 and 1.671 days and between 2.471 and 2.474 days.
B115 This star brightened by about 0.9 mag between the NSVS and Behlen photometry. The GSC magnitude is consistent with the Behlen magnitude.
B119 The NSVS data does not cover minimum light so the amplitude is a lower limit.
B127 There are significant year to year changes in the light curve, amplitude and mean magnitude. Thus, the period is poorly defined and the listed value is from the first season of the NSVS data. The photometric parameters in Table1 refer to the first season of the NSVS data. For the second season <mag> =10.09, {Delta}m=0.20, and {sigma}_m_=0.04. Table5 refers to the second season of the Behlen data. For the first season, the values were <Vmag> =10.28, <V-R> =0.60, {Delta}V=0.12 and {sigma}_V_=0.025.
B129 A shallow eclipse, {Delta}V~0.05 is possible in the Behlen data but cannot be confirmed in the NSVS data.
B145 The magnitude and scatter for the NSVS are based on data from JD=2551295 to 2551452. During the following season, JD=2551555 to 2551633, the values were <mag> =14.14 and {sigma}_m_=0.16. By the time of the Behlen photometry the magnitude was close to the earlier NSVS value so this star is likely variable on a time scale of months or years.
B146 This star has minima that suggest an eclipsing star. However, the minima are very wide, the depths vary considerably, the star reddens during each minimum and there is significant phase jitter. These factors do not support the identification as an eclipsing binary. The tabulated period is the time between successive minima,
B148 The color is uncertain as indicated by footnote o and the star is irregular so no color excess is listed.
B149 While the variation in the NSVS data is marginal, the period derived from that data produces a good light curve with small amplitude with the Behlen data. The mean magnitude faded between the NSVS and the Behlen observations but a close companion may be merged into the NSVS observation.
B151 Due to the rapid rise and phase coverage, a satisfactory Fourier fit could not be obtained. The amplitude was determined manually and the scatter was obtained with points around maximum omitted.
B152 There are significant cycle to cycle changes in the light curve, amplitude and mean magnitude. The parameters in Table5 refer to the second season of Behlen observations. In the first season <Vmag> =10.78, <V-R> =0.90, {Delta}V=0.05, and {sigma}_V_=0.02.
B167 There are two stars of similar brightness about 15" north and south of the NSVS coordinate and there are no other stars close to this location. It is very likely that they are blended in the NSVS photometry. The color and magnitude given in Table5 are the combined values from the Behlen photometry. The values for the individual stars are <Vmag> =15.97 and <Vmag> =16.10 and <V-R> =0.39 and <V-R> =0.93 for the northern and southern star, resp. A comparison of the combined magnitude and color with the NSVS magnitudes indicates that one of the two stars decreased in brightness by several tenths of a magnitude between the NSVS and the Behlen photometry. Given the individual colors it is likely that the southern star is a red variable.
B168 This star appears to have faded by about 0.2mag between the NSVS and Behlen measurements.
B170 The Behlen photometry only covers 0.1 of the cycle so variability cannot be assessed.
B172 The variation in both the NSVS data and the Behlen data is marginal. However, both occur with the same period so we have retained this star as a likely variable.
B173 There are several period aliases of similar significance between 4.212 and 4.220d. This star appears to have brightened by several tenths of a magnitude between the NSVS and the Behlen observations.
B179 Although the tabulated period fits both data sets, it produces a phase offset between them of about one half cycle.
B184 Although the light curve resembles an eclipsing binary with unequal minima, the color changes do not support this interpretation.
B188 There are several period aliases of similar significance between 45.8 and 47.2d.
B189 There are several period alias of similar significance between 3.338 and 3.345d.
B191 This star appears to have faded by about 0.2mag between the NSVS and the Behlen photometry.
B192 The four Behlen observations were clustered about maximum light so no meaningful light curve parameters could be calculated. At maximum light V=12.83 and V-R=1.10. A comparison of the Behlen and NSVS magnitudes at maximum suggest that the star became brighter by perhaps 0.4 mag between the NSVS and the Behlen observations.
B193 Observations were terminated after four data points were obtained due to the very red color of this star. All four were near maximum light so no light curve parameters could be found. At maximum light V=13.28 and V-R=1.23.
B194 This star is a known eclipsing binary (listed in the GCVS as V466 Lyr, type E:/SD:). However, the Behlen and NSVS photometry show that it exhibits a regular, stable, pulsation-like variation in addition to eclipses. The photometric parameters listed in the tables were calculated after points apparently affected by an eclipse were removed. There are 20 such points in the NSVS photometry and two in the Behlen photometry. This suggests that the eclipses occupy about 8% of the cycle, a result at odds with the SD classification. The period of the eclipses is 7.1846d (or 14.3692d if there are actually two similar eclipses present). This is close to but clearly distinct from the pulsational period, even allowing for the presence of a number of aliases of the pulsational period in the range from 7.15 to 7.20d.
B196 This star exhibited somewhat irregular variations during the NSVS observations. In particular, from JD2451274 to JD2451510 it varied in a semi-regular fashion but from JD2451600 to 2451628 it appeared to be quiescent at a magnitude of m=11.4.
B197 Observations were terminated after four data points were obtained due to the very red color of this star. All four were near maximum light so no light curve parameters could be found. At maximum light V=13.63 and V-R=2.13.
B203 There are several period aliases of similar significance between 35.2 and 36.0 days
B205 No period could be determined for the Behlen data because the star brightened nearly continuously during the 500d of observation. This contrasts with the NSVS data which contained three minima in 250d.
B208 The light curve changes between the two cycles included in the NSVS data. The photometric parameters for the NSVS data were derived from the observations before JD=2451389 that cover a little more than one cycle.
B214 The NSVS photometry may be contaminated by a fainter star about 20" away resulting in a reduction of the amplitude and apparent fading of the star between the two data sets. However, the period change cannot be explained in this way.
B225 Fairly regular variation in the NSVS data with a period of 62d. By the time of the Behlen data, 3200 days later, the regularity had been replaced by an initial rise over a few days followed by a long decline over the remaining 250 days of coverage.
B236 The large scatter in the NSVS data may be the result of eclipses but we are unable to determine a period for them and the Behlen data contain no low points.
B241 The NSVS data shows significant variation in first half of the observed interval but ceased variation after that. The NSVS magnitude during the quiescent time in reasonable agreement with the Behlen magnitude.
B242 The variation in both the NSVS data and the Behlen data is marginal. However, both occur with the same period so we have retained this star as a likely variable.
B244 Alternate minima differ. The tabulated period is the formal period between similar minima.
B245 This star appears to have faded over most of the span of the NSVS observations.
B247 No color excess is given because the variation is too irregular to determine a reliable color at the time of the spectrum.
B255 This star continually dropped in brightness over the 200 day coverage of the NSVS data.
B256 No color excess is listed because the star is too irregular for a reliable color estimation at the time of the spectrum.
B258 This star was moderately regular during the NSVS observations before JD2451500. The tabulated values of the period, <mag>, {Delta}m and {sigma}_m_ were derived from that data. After that, the last 20 NSVS data points give <mag> =11.20, {Delta}m=0.16 and {sigma}_m_=0.04.
B276 The Behlen data exhibits two minima over the 117 d cycle while the NSVS data has a single minimum and a still-stand at the phase of the second Behlen minimum.
B279 The light curve indicates an eclipsing binary with unequal eclipses and maxima that differ by about 0.1mag.
B283 Several points in both the Behlen and the NSVS data define a narrow minimum (depth about 0.34 mag, width about 0.15 cycles) superimposed on an otherwise sinusoidal light curve. A Fourier fit could not be made due to sparse coverage in the minimum.
H002 Another period, P=44.83d, is equally significant. The third season of the Behlen photometry, HD=2455798 to 2455919 was used for the determination of the period and photometric parameters. For the first season, HD=2455092 to 2455176, the magnitude at maximum matched the third season but the amplitude was about {Delta}V~0.1mag.
H006 Possibly an eclipsing binary with twice the tabulated period.
H008 Outliers, mostly in the faint direction, are present in both the NSVS and the Behlen photometry. The low outliers appear to be due to eclipses. The parameters in the table were determined with 12 low and 3 high points omitted from the NSVS photometry and 5 low points and 1 high point omitted from the Behlen photometry. Retaining those points the following values were determined: <mag> =12.66, {sigma}_m_=0.06, <Vmag> =12.93, {Delta}V=0.42, {sigma}_V_=0.079. {Delta}m and <V-R> are unaffected.
H016 The differential agreement among the three comparison stars is poor and could lead to errors in the individual light curve points at the level of about 0.02mag. The star may have brightened by about 0.1 mag between the NSVS and the Behlen observations.
H019 There are several period aliases of similar significance between 64.2 and 66.3d.
H020 This star exhibits minima of alternating depth and, to a lesser extent, maxima of alternating brightness. The tabulated period is the formal period between maxima or minima of similar magnitude. Several period aliases of similar significance are found between 2.6044 and 2.6060d. Eclipses are possible but unlikely.
H023 There are 13 low points in the NSVS data and one in the Behlen data. These may represent narrow eclipses. The photometric parameters were determined with these points omitted.
H027 There are several period aliases of similar significance in the range from 57.3 to 59.1d.
H029 About 10% of the points in the NSVS are scattered by exceptionally large amounts. This accounts for the higher than normal value of {sigma}_m_.
H034 This star was apparently constant during the first season of Behlen observations, JD=2455176 to 2455277. The data from the second and third seasons fit the same period as the NSVS data and were used to derive the tabulated values. During the first season, <Vmag> =12.22, <V-R> =0.55 and {sigma}_V_=0.019.
H035 Although the amplitude of the Behlen photometry is small, it appears to vary with the same period and similar phase as the NSVS light curve. For this reason, we treated this star to be a variable during the Behlen observations.
H037 There is no variation during the first season of the Behlen data, JD=2455170 to 2455251. The second and third seasons were used to derive the parameters in Table5. During the first season, <Vmag> =12.39, <V-R> =0.82 and {sigma}_V_=0.021.
H040 The maxima and minima vary in magnitude at the 0.1mag level in the NSVS photometry and there may be phase jitter of about 0.05 cycles.
H043 The first season of the Behlen observations, JD=2455139 to 2455257 showed very little variation and was omitted from the calculation of the photometric parameters. For that season <Vmag> =10.23, <V-R> =0.69 and {sigma}_V_=0.045.
H044 Several aliases within 0.1d of the adopted period are equally significant.
H046 A significant change in the shape of the light curve between the NSVS and the Behlen observations makes the period more uncertain than usual.
H048 There are several period aliases of similar significance between 15.29 and 15.47d.
H052 There are several aliases in the range from 14.80 to 14.98d of similar significance as the adopted period.
H054 Between the NSVS and the Behlen observations this star brightened by about 0.2mag.
H057 There are several period aliases of similar significance between 13.56 and 13.77 days.
H060 The tabulated parameters for this star were calculated without the first season of the Behlen observations, HD=2455230 to 2455295, because the amplitude was very small. During that interval, <Vmag> =13.49, <V-R> =0.65, {Delta}V=0.08 and {sigma}_V_=0.019.
H061 With the adopted period, two Behlen points near the phase of minimum are abnormally bright. This appears to be due to significant phase jitter. They were included in the calculation of the parameters in the table.
H064 In the Behlen data, the light curve has a flat maximum occupying approximately half the cycle and a symmetric minimum. Several strong aliases occur near the adopted period but they do not have a significant effect on the conclusions regarding the behavior of the star.
H066 The star increased monotonically in brightness over the 340 days of the NSVS observations.
H070 The amplitude during the first season of the Behlen observations, JD=2455295 to 2455379, is much smaller than during the later observations. The parameters in Table5 were determined using the second and third season data. For the first season <Vmag> =10.61, <V-R> =0.66, {Delta}V=0.13 and {sigma}_V_=0.019.
H071 The tabulated parameters were determined from all of the data; the large scatter is caused by significant changes in the light curve between observing seasons. For the three seasons of the Behlen photometry the mean magnitude ranges from 13.30 to 13.56, the mean color from 0.59 to 0.62, and the amplitude from 0.15 to 0.36. Similar behavior is present in the NSVS data even though it covers a smaller range of dates.
H077 The Behlen observations do not cover the maximum so no amplitude is given.
H078 The mean magnitude changed between the first and second season of the NSVS data. The tabulated values refer to the first season; during the second season <mag> =11.63, {Delta}m=0.33, and {sigma}_m_=0.023.
H080 The very steep rising branch of the light curve made it impossible to get a reasonable Fourier fit. The amplitudes, {Delta}V and {Delta}m, are just the ranges and the standard deviations, {sigma}_V_ and {sigma}_m_, were determined from the declining portion of the light curves.
H081 This star is a likely eclipsing binary. The tabulated period is the formal period between alternate similar minima.
H089 Excessive scatter in light curves suggests the presence of the Blazhko effect.
H095 This star is probably a W UMa eclipsing variable with nearly identical components. The tabulated period refers to the full cycle of two eclipses.
H098 The light curve could be interpreted as an eclipsing binary with twice the tabulated period. However, the color variation does not support this.
H099 There are several aliases between 32.25 and 32.97 of nearly equal significance.
H100 This field was only observed on a single photometric night so the zero points of the color and magnitude are questionable.
H104 This star shows alternating cycles. The tabulated period is between successive maxima and the photometric parameters were determined using it.
H119 There are several period aliases of similar significance between 58 and 60d.
H120 No period that is satisfactory for both the NSVS and the Behlen photometry could be found. There are two minima during the 1.5327 day cycle in the Behlen data or a single minimum if the period is half as great. During the 1.5323 day cycle, the NSVS data exhibits only one minimum but has excess scatter around the phase of the second minimum in the Behlen light curve. Although the minima resemble those seen in eclipsing binaries, the complex variation makes that interpretation problematic.
H127 In the NSVS photometry there are 9 low points (out of 56). These may represent narrow eclipses or simply spurious points. The NSVS parameters were determined with these points removed.
H131 This star exhibits alternating maxima of unequal brightness. The tabulated period is the formal period between two bright maxima.
H133 The shape of the light curve and the color variation strongly suggest an eclipsing binary with two nearly equal minima at a period of 49.45d.
H137 Thirty-four points in the NSVS photometry that fell more than 1.3 mag below the remainder of the data were deleted prior to analysis. No similarly faint points were found in the Behlen data so they are likely to be spurious.
H138 Ten points from the NSVS photometry fell well away from the otherwise well defined light curve. They were omitted from the determination of the photometric parameters.
H142 No period could be found that fit all of the data. The tabulated period was determined from the NSVS data and the first season of Behlen data. Several aliases of similar significance were found between 7.39 and 7.42 days. The photometric parameters in Table5 were determined from the first season of Behlen data. By the second season of the Behlen Observations, the light curve shape had changed and may have begun to exhibit a double cycle. For the second season only, <Vmag> =12.82, <V-R> =0.59, {Delta}V=0.15 and {sigma}_V_=0.019.
H144 There are several aliases in the range from 4.84 to 4.86 d with similar significance as the adopted period.
H145 Other possible periods are in the range of 36.5 to 37.6.
H146 There are several equally significant period aliases between 10.46 d and 10.54d.
H147 This star is possibly an eclipsing binary with similar minima and a period of 18.5824d. However, the color behavior does not support this interpretation.
H148 There are several period aliases of similar significance between 5.548 and 5.570d.
H154 There were only two data points during the second of the three seasons of the Behlen observations. They were not used in determining the photometric parameters because they deviated from the other data.
H157 Twenty-one outliers were removed from the 205 NSVS data points before analysis. Only {sigma}_m_ was affected significantly.
T001 Mondal et al. (2010, cat. J/AJ/139/2026) listed 29 observations of this star that give <m_TAOS_> =11.34 (arithmetic mean) with a range of 0.23mag. This star seems to exhibit occasional stillstands.
T002 Mondal et al. (2010, cat. J/AJ/139/2026) listed 29 observations of this star that give <m_TAOS_> =11.82 (intensity mean) with an amplitude of {Delta}m=0.10mag and scatter of {sigma}_m_=0.01. The star appears to be constant in the NSVS data and the cited period is based on the TAOS and Behlen data only. There are several aliases of similar significance between 60.8 and 65.5d.
T003 Mondal et al. (2010, cat. J/AJ/139/2026) listed 29 observations of this star that give <mag> =12.52 (intensity mean) with an amplitude of {Delta}m=0.13mag and scatter of {sigma}_m_=0.01. The period is based on the TAOS and Behlen data only.
T004 Mondal et al. (2010, cat. J/AJ/139/2026) listed 29 observations of this star that give <mag> =12.65 (intensity mean) with an amplitude of {Delta}m=0.11 mag and scatter of {sigma}_m_=0.01.