Unresolved from three LGGS stars >3 magnitudes fainter within 2 arcseconds.
MJD | V | * | Image | B | * | Image | R | * | Images | I | * | Images |
---|---|---|---|---|---|---|---|---|---|---|---|---|
56599.08 | 17.21± 0.03 | b | 17.16± 0.06 | b | 17.12± 0.04 | b | -- | - | - | |||
57988.34 | 17.29± 0.04 | b | 17.27± 0.04 | b | 17.20± 0.03 | b | 17.18± 0.04 | b | ||||
58077.11 | 17.14± 0.06 | b | 17.14± 0.05 | b | 17.05± 0.05 | b | 17.17± 0.07 | b | ||||
58342.31 | 17.02± 0.04 | b | -- | - | - | -- | - | - | 17.15± 0.05 | b | ||
58372.15 | 17.01± 0.04 | b | -- | - | - | -- | - | - | 16.95± 0.05 | b | ||
58671.33 | 17.03± 0.05 | b | 17.00± 0.05 | b | -- | - | - | -- | - | - | ||
58696.25 | 16.96± 0.05 | b | 16.97± 0.05 | b | 16.91± 0.04 | b | 16.98± 0.04 | b | ||||
59019.35 | 17.00± 0.04 | b | 16.98± 0.04 | b | -- | - | - | -- | - | - | ||
59059.34 | 17.09± 0.04 | b | -- | - | - | 16.99± 0.03 | b | -- | - | - | ||
59077.17 | 17.01± 0.05 | b | -- | - | - | -- | - | - | 16.98± 0.04 | b | ||
59082.22 | 16.99± 0.04 | b | 16.96± 0.05 | b | -- | - | - | -- | - | - | ||
59136.09 | 16.93± 0.04 | b | 16.92± 0.04 | b | 16.90± 0.04 | b | -- | - | - | |||
59166.10 | 16.94± 0.04 | b | -- | - | - | -- | - | - | 16.94± 0.04 | b | ||
59379.36 | 16.94± 0.05 | b | -- | - | - | 16.88± 0.04 | b | -- | - | - | ||
59442.24 | 17.23± 0.05 | b | 17.14± 0.04 | b | -- | - | - | 17.05± 0.04 | b | |||
59483.09 | 16.91± 0.05 | b | -- | - | - | 16.88± 0.04 | b | -- | - | - | ||
59525.08 | 17.29± 0.05 | b | 17.21± 0.05 | b | -- | - | - | -- | - | - | ||
59546.11 | 17.02± 0.04 | b | -- | - | - | -- | - | - | 17.03± 0.04 | b | ||
59753.38 | 17.07± 0.04 | b | 17.11± 0.06 | b | 17.01± 0.03 | b | -- | - | - | |||
59823.12 | 16.97± 0.05 | b | -- | - | - | -- | - | - | 16.90± 0.05 | b | ||
59854.11 | 17.09± 0.04 | b | 17.07± 0.04 | b | 17.03± 0.04 | b | -- | - | - | |||
59905.15 | 16.97± 0.04 | b | 16.94± 0.06 | b | 16.92± 0.04 | b | 16.90± 0.06 | 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 [0.35 mag] | B [0.38 mag] | R [0.33 mag] | |
---|---|---|---|
B [0.35 mag] | 0.93 (13) | ||
R [0.33 mag] | 0.98 (11) | 0.94 (8) | |
I [0.28 mag] | 0.52 (11) | 0.83 (5) | 0.75 (4) |
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) | 7.31 | 0.85 | ||
R (I|R) | 9.03 | 0.98 | 8.32 | 0.75 | |
I (I|R) | 4.55 | 1.16 | 6.29 | 1.13 | --- | ---- |
By John C. Martin, University of Illinois Springfield Henry R. Barber Research Observatory
Generated on 2023-08-14 14:15:12 UT-5