On the edge of but separated by 4 arcseconds from a group of LGGS stars >2 magnitudes fainter. Indicated in individual records when unresolved by bad seeing.
MJD | V | * | Image | B | * | Image | R | * | Images | I | * | Images |
---|---|---|---|---|---|---|---|---|---|---|---|---|
56140.40 | 17.52± 0.06 | b | -- | - | - | 17.09± 0.09 | X | -- | - | - | ||
56599.22 | 17.82± 0.09 | X | 17.89± 0.05 | b | 17.14± 0.06 | b | -- | - | - | |||
56982.22 | 17.41± 0.06 | b | 17.94± 0.06 | b | 17.01± 0.07 | b | -- | - | - | |||
57035.14 | 17.34± 0.04 | b | 17.83± 0.05 | b | 17.08± 0.05 | b | -- | - | - | |||
57310.16 | 17.75± 0.07 | X | 17.95± 0.05 | b | 16.97± 0.05 | b | -- | - | - | |||
57328.19 | 17.48± 0.05 | b | 17.99± 0.07 | b | 17.05± 0.07 | b | -- | - | - | |||
57406.10 | 17.27± 0.05 | b | 17.88± 0.08 | b | 17.01± 0.05 | b | 16.61± 0.07 | b | ||||
57634.41 | 17.39± 0.07 | b | 17.93± 0.08 | b | 16.91± 0.08 | b | -- | - | - | |||
57638.40 | 17.48± 0.05 | Ab | 18.07± 0.05 | b | 17.06± 0.04 | b | 16.71± 0.08 | Ab | ||||
57988.43 | 17.43± 0.06 | Tb | -- | - | - | -- | - | - | -- | - | - | |
58043.15 | 17.44± 0.04 | Ab | 17.92± 0.05 | Ab | 16.92± 0.06 | Ab | 16.63± 0.09 | b | ||||
58108.17 | 17.39± 0.05 | b | 17.79± 0.06 | b | -- | - | - | 16.60± 0.09 | b | |||
58339.40 | 17.33± 0.05 | b | 17.85± 0.06 | b | 16.95± 0.06 | b | -- | - | - | |||
58375.16 | 17.48± 0.05 | b | -- | - | - | -- | - | - | 16.70± 0.10 | b | ||
58433.02 | 17.54± 0.05 | b | -- | - | - | 17.12± 0.05 | b | 16.73± 0.11 | b | |||
58673.38 | 17.54± 0.03 | b | 18.16± 0.04 | b | -- | - | - | -- | - | - | ||
58695.39 | 17.55± 0.05 | b | -- | - | - | 17.16± 0.04 | b | -- | - | - | ||
58696.41 | 17.55± 0.05 | b | 18.14± 0.08 | b | 17.12± 0.07 | b | -- | - | - | |||
58750.22 | 17.51± 0.05 | b | 18.04± 0.04 | b | -- | - | - | 16.79± 0.08 | b | |||
58757.17 | 17.50± 0.06 | b | -- | - | - | 17.12± 0.05 | b | -- | - | - | ||
58784.14 | 17.54± 0.05 | Ab | -- | - | - | 17.10± 0.05 | b | 16.82± 0.08 | b | |||
58812.20 | 17.45± 0.06 | b | -- | - | - | 17.00± 0.07 | b | -- | - | - | ||
59059.40 | 17.60± 0.06 | b | -- | - | - | 17.18± 0.05 | b | 16.89± 0.09 | b | |||
59081.34 | 17.63± 0.05 | Ab | 18.07± 0.05 | Ab | 17.19± 0.05 | Ab | 16.78± 0.08 | b | ||||
59082.35 | 17.61± 0.04 | Ab | 18.15± 0.03 | Ab | 17.19± 0.04 | Ab | -- | - | - | |||
59084.25 | -- | - | - | -- | - | - | 17.19± 0.04 | Tb | -- | - | - | |
59161.12 | 17.40± 0.04 | Ab | 17.81± 0.03 | b | 16.99± 0.05 | Ab | 16.71± 0.09 | b | ||||
59171.14 | 17.48± 0.05 | Ab | 17.93± 0.06 | Ab | 17.04± 0.05 | b | 16.70± 0.08 | Ab | ||||
59227.14 | 17.61± 0.05 | Ab | 18.09± 0.05 | Ab | 17.17± 0.05 | Ab | 16.83± 0.08 | b | ||||
59415.38 | 17.55± 0.05 | Ab | 18.02± 0.05 | b | -- | - | - | -- | - | - | ||
59441.42 | 17.48± 0.06 | Tb | -- | - | - | -- | - | - | -- | - | - | |
59442.40 | 17.50± 0.04 | Ab | -- | - | - | 17.10± 0.05 | Ab | 16.68± 0.08 | b | |||
59463.33 | 17.53± 0.06 | Ab | 18.02± 0.07 | Ab | -- | - | - | 16.78± 0.07 | b | |||
59522.13 | 17.40± 0.05 | b | -- | - | - | 17.02± 0.05 | b | 16.75± 0.09 | b | |||
59525.15 | 17.38± 0.04 | Ab | -- | - | - | 17.07± 0.04 | b | 16.53± 0.09 | b | |||
59546.19 | 17.43± 0.04 | Ab | 17.93± 0.03 | b | 17.00± 0.05 | b | 16.74± 0.08 | b | ||||
59551.14 | 17.40± 0.06 | Ab | 17.79± 0.04 | b | -- | - | - | 16.72± 0.08 | b | |||
59583.18 | 17.53± 0.04 | Ab | -- | - | - | 17.12± 0.05 | b | 16.80± 0.08 | b | |||
59608.12 | 17.49± 0.05 | Ab | 17.89± 0.08 | b | 17.11± 0.07 | Ab | -- | - | - |
If the brightness variation is true variability then there should be a correlation between brightness changes recorded in different filter bands. The following table are the R-squared linear correlation factors calculated for the pairs of bands. The number in parentheses next to the R-squared value is the number of elements used to calculate the correlation factor. The number in square brackets next to the band is the range of magnitudes measured.
V [0.37 mag] | B [0.35 mag] | R [0.28 mag] | |
---|---|---|---|
B [0.37 mag] | 0.68 (22) | ||
R [0.28 mag] | 0.62 (26) | 0.36 (18) | |
I [0.35 mag] | 0.60 (20) | 0.47 (12) | 0.37 (15) |
The plots below are provided to check the values in the table above and also to show any non-linear correlations
Welch & Stetson (1993, AJ, 105, 1813) present a method for varible star detection in CCD images from automated surveys. Data from two bands are compared and two statistics are calculated: R and I.
The I-statistic has an expectation value of zero for stars that are NOT variable. A larger non-zero I-value indicates a higher likelihood that the star is variable. The R statistic indicates how the color of the star changes as the variable grows brighter with R = 1.0 being no change in color.
R and I values have only been calculated if there are more than four (4) matched measurements of brightness in each band.
V (I|R) | B (I|R) | R (I|R) | |
---|---|---|---|
B (I|R) | 4.21 | 1.30 | ||
R (I|R) | 2.15 | 1.26 | -0.35 | 0.10 | |
I (I|R) | 1.44 | 1.81 | 1.34 | 2.92 | 0.95 | 1.48 |
By John C. Martin, University of Illinois Springfield Henry R. Barber Research Observatory
Generated on 2023-08-14 14:15:12 UT-5