Unresolved from LGGS star J013307.63+304259.2 two magnitudes fainter in V and comparable brightness in BRI. Also difficult to separate from a pair of LGGS stars J013307.50+304258.5 A and B which are at least one magnitude brighter 1.4 arcseconds WSW.
MJD | V | * | Image | B | * | Image | R | * | Images | I | * | Images |
---|---|---|---|---|---|---|---|---|---|---|---|---|
56140.39 | 16.91± 0.04 | B | -- | - | - | 16.31± 0.08 | B | -- | - | - | ||
56593.16 | 17.30± 0.04 | B | 17.19± 0.03 | B | -- | - | - | -- | - | - | ||
56599.19 | 17.24± 0.04 | B | 17.20± 0.03 | B | 17.09± 0.06 | B | -- | - | - | |||
56976.19 | 16.99± 0.04 | B | 17.14± 0.04 | B | 16.54± 0.07 | B | -- | - | - | |||
57328.16 | 17.09± 0.03 | B | 17.19± 0.04 | B | 16.59± 0.04 | B | -- | - | - | |||
57634.38 | 17.06± 0.04 | B | 17.20± 0.05 | B | 16.52± 0.06 | B | 15.65± 0.08 | B | ||||
57964.40 | 16.90± 0.04 | B | -- | - | - | -- | - | - | 15.23± 0.07 | AB | ||
57988.41 | 16.87± 0.04 | B | 17.08± 0.04 | B | -- | - | - | -- | - | - | ||
58043.11 | 16.87± 0.04 | AB | 17.14± 0.04 | B | 16.22± 0.05 | AB | 15.22± 0.06 | B | ||||
58073.22 | 16.86± 0.05 | B | 17.14± 0.04 | B | -- | - | - | -- | - | - | ||
58103.17 | 16.92± 0.04 | B | 17.19± 0.04 | B | -- | - | - | -- | - | - | ||
58108.11 | 16.94± 0.05 | AB | 17.16± 0.05 | AB | -- | - | - | 15.30± 0.07 | AB | |||
58316.35 | 17.09± 0.04 | B | 17.25± 0.04 | B | -- | - | - | -- | - | - | ||
58341.37 | 17.02± 0.04 | B | -- | - | - | -- | - | - | 15.49± 0.08 | B | ||
58373.15 | 16.91± 0.06 | B | 17.21± 0.07 | B | -- | - | - | -- | - | - | ||
58433.02 | 16.84± 0.05 | B | -- | - | - | 16.27± 0.05 | B | 15.44± 0.10 | B | |||
58673.38 | 17.02± 0.03 | B | 17.26± 0.03 | B | -- | - | - | -- | - | - | ||
58750.19 | 16.98± 0.04 | B | -- | - | - | 16.32± 0.05 | B | -- | - | - | ||
58779.18 | 16.80± 0.04 | B | 17.08± 0.03 | B | -- | - | - | -- | - | - | ||
58812.20 | 16.93± 0.06 | B | -- | - | - | 16.26± 0.06 | B | -- | - | - | ||
58902.05 | 16.94± 0.03 | B | -- | - | - | -- | - | - | 15.37± 0.07 | B | ||
59056.38 | 16.91± 0.04 | B | 17.08± 0.06 | B | 16.36± 0.05 | B | 15.44± 0.07 | B | ||||
59082.32 | 17.08± 0.03 | B | 17.28± 0.04 | B | 16.48± 0.04 | B | -- | - | - | |||
59084.29 | -- | - | - | -- | - | - | 16.45± 0.05 | TB | -- | - | - | |
59161.11 | 17.11± 0.03 | B | 17.16± 0.03 | B | 16.48± 0.05 | B | -- | - | - | |||
59171.11 | 17.02± 0.03 | B | 17.14± 0.03 | B | -- | - | - | 15.49± 0.08 | B | |||
59227.10 | 17.01± 0.03 | B | 17.17± 0.03 | B | -- | - | - | -- | - | - | ||
59415.38 | 17.04± 0.03 | B | 17.18± 0.03 | B | -- | - | - | -- | - | - | ||
59442.39 | 16.98± 0.03 | B | -- | - | - | 16.50± 0.05 | B | 15.71± 0.08 | B | |||
59523.17 | 17.06± 0.03 | B | 17.19± 0.03 | B | -- | - | - | -- | - | - | ||
59525.17 | 17.17± 0.03 | B | -- | - | - | -- | - | - | 15.90± 0.10 | B | ||
59546.17 | 17.07± 0.03 | B | -- | - | - | 16.61± 0.04 | - | -- | - | - | ||
59551.15 | 17.17± 0.03 | B | 17.13± 0.03 | B | -- | - | - | -- | - | - | ||
59583.16 | 17.06± 0.03 | B | -- | - | - | -- | - | - | 15.74± 0.08 | B | ||
59608.10 | 17.06± 0.05 | B | -- | - | - | 16.48± 0.04 | B | -- | - | - |
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 [0.20 mag] | B [0.50 mag] | R [0.88 mag] | |
---|---|---|---|
B [0.20 mag] | 0.22 (22) | ||
R [0.88 mag] | 0.77 (15) | 0.13 (8) | |
I [0.68 mag] | 0.68 (12) | 0.13 (5) | 0.89 (5) |
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) | 1.97 | 0.43 | ||
R (I|R) | 8.37 | 0.89 | 1.79 | 0.08 | |
I (I|R) | 5.27 | 0.95 | 0.63 | 0.32 | 5.81 | 1.02 |
By John C. Martin, University of Illinois Springfield Henry R. Barber Research Observatory
Generated on 2023-08-14 14:15:12 UT-5