Fifteen other LGGS stars within 5 arcseconds (most >3 magnitudes fainter.
MJD | V | * | Image | B | * | Image | R | * | Images | I | * | Images |
---|---|---|---|---|---|---|---|---|---|---|---|---|
56593.14 | 16.73± 0.04 | b | 17.40± 0.05 | b | 16.15± 0.06 | b | -- | - | - | |||
56599.11 | 16.71± 0.03 | b | 17.43± 0.10 | b | 16.16± 0.04 | b | -- | - | - | |||
56930.14 | 16.64± 0.03 | b | 17.31± 0.04 | b | 16.07± 0.04 | b | -- | - | - | |||
57285.24 | 16.79± 0.05 | b | 17.36± 0.04 | b | 16.19± 0.05 | b | -- | - | - | |||
57340.19 | 16.76± 0.06 | b | -- | - | - | -- | - | - | 15.91± 0.08 | b | ||
57635.27 | 16.69± 0.04 | b | 17.43± 0.04 | b | 16.16± 0.04 | b | 15.92± 0.04 | b | ||||
57743.06 | 16.71± 0.03 | b | 17.41± 0.04 | b | 16.18± 0.04 | b | 15.91± 0.05 | b | ||||
57963.32 | 16.79± 0.05 | b | 17.48± 0.06 | b | -- | - | - | 15.96± 0.07 | b | |||
58035.05 | 16.76± 0.05 | b | -- | - | - | 16.22± 0.06 | b | -- | - | - | ||
58073.10 | 16.72± 0.06 | b | 17.37± 0.06 | b | -- | - | - | -- | - | - | ||
58098.16 | 16.76± 0.05 | b | -- | - | - | 16.18± 0.05 | b | 15.92± 0.07 | b | |||
58312.37 | 16.75± 0.06 | b | 17.45± 0.08 | b | -- | - | - | -- | - | - | ||
58339.30 | 16.79± 0.06 | b | -- | - | - | 16.24± 0.06 | b | 15.95± 0.07 | b | |||
58342.29 | 16.78± 0.05 | b | 17.50± 0.07 | b | -- | - | - | -- | - | - | ||
58373.11 | 16.77± 0.05 | b | 17.44± 0.07 | b | -- | - | - | -- | - | - | ||
58673.32 | 16.80± 0.03 | b | 17.54± 0.04 | b | -- | - | - | -- | - | - | ||
58750.16 | 16.77± 0.03 | b | -- | - | - | 16.23± 0.04 | b | 15.95± 0.06 | b | |||
58784.10 | 16.80± 0.03 | b | 17.57± 0.04 | b | -- | - | - | -- | - | - | ||
58836.15 | 16.74± 0.04 | X | -- | - | - | 16.14± 0.04 | b | 15.94± 0.06 | b | |||
59026.35 | 16.78± 0.06 | b | -- | - | - | 16.25± 0.06 | b | -- | - | - | ||
59056.32 | 16.83± 0.04 | Ab | 17.50± 0.04 | Ab | -- | - | - | 15.90± 0.06 | b | |||
59081.17 | 16.87± 0.03 | b | -- | - | - | 16.30± 0.04 | b | 16.01± 0.04 | b | |||
59082.26 | 16.78± 0.04 | b | 17.47± 0.05 | b | 16.16± 0.05 | b | -- | - | - | |||
59131.13 | 16.87± 0.03 | b | 17.51± 0.03 | b | -- | - | - | -- | - | - | ||
59136.05 | 16.72± 0.04 | b | -- | - | - | -- | - | - | 15.89± 0.06 | b | ||
59166.18 | 16.74± 0.04 | b | 17.41± 0.05 | b | 16.17± 0.04 | b | -- | - | - | |||
59194.14 | 16.85± 0.03 | b | -- | - | - | 16.32± 0.04 | b | -- | - | - | ||
59382.36 | 16.70± 0.04 | b | -- | - | - | 16.09± 0.05 | b | -- | - | - | ||
59415.30 | 16.80± 0.04 | b | 17.51± 0.05 | b | -- | - | - | -- | - | - | ||
59441.30 | 16.75± 0.04 | b | 17.53± 0.06 | b | -- | - | - | -- | - | - | ||
59463.19 | 16.81± 0.04 | Ab | -- | - | - | 16.17± 0.05 | b | 15.95± 0.06 | Ab | |||
59485.10 | 17.03± 0.05 | b | 17.65± 0.05 | b | 16.31± 0.04 | b | -- | - | - | |||
59523.10 | 16.68± 0.04 | b | 17.61± 0.11 | b | -- | - | - | -- | - | - | ||
59548.06 | 16.72± 0.03 | Ab | 17.43± 0.03 | b | 16.13± 0.04 | Ab | 15.82± 0.06 | b | ||||
59794.25 | 16.71± 0.04 | b | 17.47± 0.06 | b | -- | - | - | -- | - | - | ||
59823.16 | 16.84± 0.04 | Ab | 17.43± 0.06 | b | 16.34± 0.05 | b | -- | - | - | |||
59849.08 | 16.70± 0.06 | b | -- | - | - | -- | - | - | 15.85± 0.06 | b | ||
59904.06 | 16.66± 0.04 | b | -- | - | - | 16.07± 0.04 | b | 15.78± 0.06 | b | |||
59932.10 | 16.64± 0.04 | b | 17.37± 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 [0.34 mag] | B [0.39 mag] | R [0.27 mag] | |
---|---|---|---|
B [0.34 mag] | 0.36 (25) | ||
R [0.27 mag] | 0.66 (21) | 0.40 (11) | |
I [0.23 mag] | 0.61 (14) | 0.10 (5) | 0.73 (10) |
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) | 2.51 | 0.86 | ||
R (I|R) | 3.45 | 1.11 | -0.30 | 0.04 | |
I (I|R) | 1.36 | 1.66 | 0.16 | 1.20 | 1.68 | 1.36 |
By John C. Martin, University of Illinois Springfield Henry R. Barber Research Observatory
Generated on 2023-08-14 14:15:12 UT-5