Unresolved from three LGGS stars combined to be about one magnitude fainter 1 arcsecond E.
MJD | V | * | Image | B | * | Image | R | * | Images | I | * | Images |
---|---|---|---|---|---|---|---|---|---|---|---|---|
56140.40 | 16.96± 0.05 | B | -- | - | - | 16.85± 0.08 | B | -- | - | - | ||
56599.22 | 16.81± 0.06 | B | 16.82± 0.04 | B | 16.66± 0.05 | B | -- | - | - | |||
56982.22 | 16.95± 0.06 | B | 16.92± 0.06 | B | 16.82± 0.07 | B | -- | - | - | |||
57310.16 | 17.00± 0.06 | B | 16.92± 0.04 | B | 16.69± 0.05 | B | -- | - | - | |||
57328.19 | 16.98± 0.05 | B | 16.95± 0.07 | B | 16.82± 0.07 | B | -- | - | - | |||
57634.41 | 17.09± 0.06 | B | 17.08± 0.08 | B | 16.93± 0.08 | B | -- | - | - | |||
57638.43 | 17.06± 0.06 | B | -- | - | - | -- | - | - | 16.83± 0.10 | B | ||
57964.33 | 16.97± 0.04 | B | 16.99± 0.07 | B | 16.87± 0.05 | B | 16.74± 0.06 | B | ||||
57988.43 | 16.98± 0.06 | TB | -- | - | - | -- | - | - | -- | - | - | |
58043.16 | 16.93± 0.04 | B | 16.95± 0.06 | B | 16.79± 0.06 | B | 16.65± 0.09 | B | ||||
58108.17 | 16.89± 0.05 | B | 16.90± 0.05 | B | -- | - | - | 16.62± 0.09 | B | |||
58317.37 | 17.00± 0.04 | B | 17.03± 0.07 | B | 16.87± 0.04 | B | -- | - | - | |||
58339.40 | 16.96± 0.05 | B | 17.00± 0.06 | B | 16.82± 0.06 | B | -- | - | - | |||
58375.16 | 17.00± 0.05 | B | -- | - | - | -- | - | - | 16.73± 0.09 | B | ||
58696.41 | 17.07± 0.05 | B | 17.09± 0.07 | B | 16.93± 0.07 | B | -- | - | - | |||
58757.17 | 17.00± 0.05 | B | -- | - | - | 16.85± 0.05 | B | -- | - | - | ||
58784.15 | 17.02± 0.05 | B | -- | - | - | -- | - | - | 16.75± 0.08 | B | ||
59081.36 | 16.95± 0.05 | B | 16.94± 0.05 | B | 16.80± 0.05 | B | 16.58± 0.07 | B | ||||
59084.38 | -- | - | - | -- | - | - | 16.83± 0.07 | TB | -- | - | - | |
59171.17 | 16.91± 0.04 | B | 16.87± 0.08 | B | 16.76± 0.05 | B | 16.65± 0.08 | B | ||||
59227.15 | 16.95± 0.05 | B | 16.93± 0.06 | B | 16.80± 0.04 | B | 16.66± 0.07 | B | ||||
59441.42 | 16.98± 0.06 | TB | -- | - | - | -- | - | - | -- | - | - | |
59463.34 | 17.00± 0.06 | B | 16.99± 0.08 | B | -- | - | - | -- | - | - | ||
59522.13 | 16.84± 0.05 | B | -- | - | - | 16.70± 0.05 | B | 16.60± 0.08 | B | |||
59546.22 | 17.05± 0.06 | B | -- | - | - | -- | - | - | 16.80± 0.08 | B | ||
59551.16 | 17.03± 0.07 | TB | -- | - | - | -- | - | - | -- | - | - | |
59608.14 | 17.03± 0.05 | B | 17.02± 0.07 | B | 16.86± 0.05 | 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 [0.27 mag] | B [0.27 mag] | R [0.27 mag] | |
---|---|---|---|
B [0.27 mag] | 0.82 (16) | ||
R [0.27 mag] | 0.66 (17) | 0.83 (14) | |
I [0.26 mag] | 0.76 (11) | 0.26 (6) | 0.51 (6) |
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) | 1.25 | 1.01 | ||
R (I|R) | 1.31 | 0.86 | 1.29 | 0.39 | |
I (I|R) | 1.10 | 1.18 | 0.23 | 0.81 | 0.60 | 1.21 |
By John C. Martin, University of Illinois Springfield Henry R. Barber Research Observatory
Generated on 2023-08-14 14:15:12 UT-5