One LGGS star 2 magnitudes fainter 4 arcseconds to S does not interfere sigificantly with PSF fit. Seven other LGGS stars >3.5 magnitudes fainter within 5 arcseconds.
MJD | V | * | Image | B | * | Image | R | * | Images | I | * | Images |
---|---|---|---|---|---|---|---|---|---|---|---|---|
56142.33 | 17.41± 0.06 | Tb | -- | - | - | -- | - | - | -- | - | - | |
56267.15 | -- | - | - | -- | - | - | 17.00± 0.05 | Tb | -- | - | - | |
56490.38 | 17.40± 0.04 | Tb | -- | - | - | -- | - | - | -- | - | - | |
56536.26 | 17.46± 0.05 | b | -- | - | - | 17.00± 0.06 | b | -- | - | - | ||
56537.18 | 17.49± 0.04 | Ab | 17.95± 0.06 | Ab | 17.13± 0.04 | b | -- | - | - | |||
56915.16 | 17.51± 0.04 | b | 17.89± 0.06 | b | 17.02± 0.05 | b | -- | - | - | |||
57227.34 | 17.50± 0.04 | b | 17.95± 0.05 | b | 16.99± 0.04 | b | -- | - | - | |||
57310.10 | 17.46± 0.04 | b | -- | - | - | -- | - | - | 16.70± 0.07 | b | ||
57633.35 | 17.42± 0.05 | Ab | 17.87± 0.06 | Ab | 16.96± 0.05 | Ab | -- | - | - | |||
57635.35 | 17.44± 0.05 | b | -- | - | - | -- | - | - | 16.66± 0.06 | b | ||
57638.25 | 17.43± 0.04 | b | -- | - | - | -- | - | - | 16.70± 0.07 | b | ||
57888.07 | 17.58± 0.10 | X | 17.99± 0.21 | X | 16.90± 0.08 | X | -- | - | - | |||
57928.32 | 17.34± 0.04 | b | 17.80± 0.07 | b | 16.84± 0.06 | b | 16.49± 0.08 | b | ||||
57958.26 | 17.56± 0.06 | b | 17.93± 0.08 | b | -- | - | - | 16.73± 0.06 | b | |||
57963.26 | 17.42± 0.06 | b | 17.83± 0.07 | b | -- | - | - | -- | - | - | ||
57988.22 | 17.53± 0.07 | b | 18.00± 0.08 | b | -- | - | - | 16.61± 0.06 | b | |||
58035.03 | 17.45± 0.04 | b | -- | - | - | 16.99± 0.04 | b | -- | - | - | ||
58043.05 | 17.52± 0.05 | b | 17.98± 0.06 | b | 17.03± 0.04 | b | -- | - | - | |||
58045.05 | 17.52± 0.05 | b | -- | - | - | -- | - | - | 16.73± 0.07 | b | ||
58067.10 | 17.38± 0.05 | b | -- | - | - | -- | - | - | 16.63± 0.06 | b | ||
58073.09 | 17.49± 0.06 | b | 17.88± 0.07 | b | -- | - | - | -- | - | - | ||
58077.08 | 17.44± 0.07 | b | -- | - | - | -- | - | - | 16.73± 0.07 | b | ||
58098.07 | 17.36± 0.06 | b | 17.85± 0.07 | b | -- | - | - | -- | - | - | ||
58103.08 | 17.43± 0.05 | b | -- | - | - | -- | - | - | 16.61± 0.07 | b | ||
58312.26 | 17.55± 0.06 | b | 18.04± 0.08 | b | 17.05± 0.06 | b | -- | - | - | |||
58316.24 | 17.49± 0.06 | b | -- | - | - | -- | - | - | 16.62± 0.06 | b | ||
58339.26 | 17.51± 0.07 | b | -- | - | - | -- | - | - | 16.68± 0.07 | b | ||
58342.26 | 17.49± 0.04 | b | 17.90± 0.07 | b | -- | - | - | -- | - | - | ||
58366.11 | 17.45± 0.04 | b | 17.85± 0.07 | b | -- | - | - | -- | - | - | ||
58375.09 | 17.45± 0.05 | b | -- | - | - | 17.01± 0.04 | b | -- | - | - | ||
58403.06 | 17.34± 0.04 | b | -- | - | - | -- | - | - | 16.56± 0.05 | b | ||
58420.01 | 17.33± 0.06 | b | 17.74± 0.08 | b | -- | - | - | -- | - | - | ||
58436.04 | 17.36± 0.04 | b | 17.73± 0.06 | b | 16.83± 0.04 | b | -- | - | - | |||
58671.35 | 17.39± 0.03 | Ab | 17.83± 0.04 | b | 16.96± 0.04 | b | -- | - | - | |||
58695.41 | 17.53± 0.03 | b | -- | - | - | 17.01± 0.04 | b | -- | - | - | ||
58750.11 | 17.35± 0.04 | b | -- | - | - | -- | - | - | 16.54± 0.05 | b | ||
58779.03 | 17.36± 0.03 | b | 17.80± 0.03 | b | -- | - | - | -- | - | - | ||
58812.16 | 17.40± 0.03 | b | -- | - | - | 16.91± 0.04 | b | -- | - | - | ||
59000.37 | 17.44± 0.06 | b | -- | - | - | 17.00± 0.05 | b | -- | - | - | ||
59055.29 | 17.42± 0.06 | b | 17.90± 0.07 | b | -- | - | - | -- | - | - | ||
59077.25 | 17.45± 0.07 | b | -- | - | - | 16.97± 0.05 | b | 16.65± 0.06 | b | |||
59131.11 | 17.43± 0.05 | b | 17.95± 0.05 | b | -- | - | - | -- | - | - | ||
59166.14 | 17.40± 0.05 | b | -- | - | - | -- | - | - | 16.66± 0.06 | b | ||
59194.12 | 17.46± 0.04 | b | -- | - | - | 16.96± 0.05 | b | -- | - | - | ||
59376.38 | 17.46± 0.07 | b | 17.94± 0.07 | b | -- | - | - | -- | - | - | ||
59409.33 | 17.68± 0.11 | AX | -- | - | - | 17.02± 0.06 | b | -- | - | - | ||
59442.36 | 17.40± 0.06 | b | 17.82± 0.07 | b | -- | - | - | 16.60± 0.06 | b | |||
59467.13 | 17.46± 0.07 | b | -- | - | - | 17.05± 0.04 | b | -- | - | - | ||
59522.10 | 17.42± 0.04 | b | 17.85± 0.06 | b | -- | - | - | -- | - | - | ||
59546.13 | 17.47± 0.04 | b | -- | - | - | -- | - | - | 16.70± 0.06 | b | ||
59583.12 | 17.32± 0.05 | b | -- | - | - | 16.92± 0.04 | b | -- | - | - | ||
59739.38 | 17.41± 0.06 | b | 17.86± 0.07 | b | 16.90± 0.05 | b | -- | - | - | |||
59816.16 | 17.46± 0.06 | b | -- | - | - | 16.98± 0.04 | b | -- | - | - | ||
59848.09 | 17.36± 0.04 | b | -- | - | - | -- | - | - | 16.50± 0.06 | b | ||
59879.05 | 17.38± 0.05 | b | 17.88± 0.07 | b | -- | - | - | -- | - | - | ||
59905.10 | 17.46± 0.04 | b | -- | - | - | 17.01± 0.03 | b | 16.71± 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 [0.31 mag] | B [0.24 mag] | R [0.30 mag] | |
---|---|---|---|
B [0.31 mag] | 0.71 (25) | ||
R [0.30 mag] | 0.64 (22) | 0.72 (10) | |
I [0.24 mag] | 0.52 (20) | 0.38 (4) | 1.00 (3) |
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) | 1.36 | 0.83 | ||
R (I|R) | 1.59 | 0.90 | 0.69 | 0.06 | |
I (I|R) | 1.29 | 1.16 | --- | --- | --- | ---- |
By John C. Martin, University of Illinois Springfield Henry R. Barber Research Observatory
Generated on 2023-08-14 14:15:12 UT-5