Not resolved from J013242.31+302113.9 of comparable brightness less than one arcsecond SE.
MJD | V | * | Image | B | * | Image | R | * | Images | I | * | Images |
---|---|---|---|---|---|---|---|---|---|---|---|---|
56140.40 | 18.22± 0.07 | B | -- | - | - | 17.09± 0.09 | B | -- | - | - | ||
56599.22 | 18.07± 0.07 | B | 18.58± 0.07 | B | 17.03± 0.06 | B | -- | - | - | |||
57035.14 | 18.03± 0.05 | B | 18.59± 0.09 | B | 17.05± 0.05 | B | -- | - | - | |||
57310.16 | 18.02± 0.06 | B | 18.69± 0.06 | B | 17.13± 0.05 | B | -- | - | - | |||
57638.39 | 18.38± 0.04 | B | 18.96± 0.06 | B | 17.45± 0.04 | B | 16.53± 0.07 | B | ||||
57988.43 | 18.11± 0.06 | TB | -- | - | - | -- | - | - | -- | - | - | |
58043.16 | 18.13± 0.05 | B | 18.73± 0.07 | B | 17.13± 0.06 | B | 16.25± 0.09 | B | ||||
58108.17 | 18.23± 0.06 | B | 18.72± 0.06 | B | -- | - | - | 16.38± 0.09 | B | |||
58339.40 | 18.26± 0.06 | B | 18.81± 0.08 | B | 17.31± 0.06 | B | -- | - | - | |||
58375.16 | 18.23± 0.06 | B | -- | - | - | -- | - | - | 16.31± 0.09 | B | ||
58695.39 | 18.25± 0.05 | B | -- | - | - | 17.31± 0.04 | B | -- | - | - | ||
58750.22 | 18.34± 0.05 | B | 18.89± 0.05 | B | -- | - | - | 16.47± 0.08 | B | |||
58784.14 | 18.26± 0.05 | B | -- | - | - | 17.38± 0.05 | B | -- | - | - | ||
59081.36 | 18.14± 0.06 | B | 18.68± 0.06 | B | 17.19± 0.05 | B | 16.29± 0.07 | B | ||||
59082.38 | 18.12± 0.06 | B | 18.81± 0.04 | B | 17.24± 0.04 | B | -- | - | - | |||
59084.25 | -- | - | - | -- | - | - | 17.25± 0.04 | TB | -- | - | - | |
59161.14 | 18.27± 0.05 | B | -- | - | - | 17.34± 0.04 | B | 16.45± 0.09 | B | |||
59171.15 | 18.29± 0.06 | AB | 18.68± 0.07 | AB | 17.36± 0.05 | B | 16.44± 0.08 | AB | ||||
59227.14 | 18.18± 0.05 | AB | 18.75± 0.06 | AB | 17.25± 0.05 | AB | 16.32± 0.07 | B | ||||
59415.39 | 18.34± 0.08 | TB | -- | - | - | -- | - | - | -- | - | - | |
59441.42 | 18.17± 0.07 | TB | -- | - | - | -- | - | - | -- | - | - | |
59442.41 | 18.22± 0.06 | B | -- | - | - | 17.26± 0.04 | B | -- | - | - | ||
59463.33 | 18.24± 0.06 | AB | 18.75± 0.07 | AB | -- | - | - | 16.37± 0.07 | B | |||
59522.13 | 18.24± 0.05 | B | -- | - | - | 17.28± 0.05 | B | 16.34± 0.08 | B | |||
59525.12 | 18.19± 0.06 | B | -- | - | - | 17.28± 0.04 | B | -- | - | - | ||
59546.20 | 18.23± 0.05 | AB | 18.80± 0.04 | B | -- | - | - | 16.32± 0.07 | B | |||
59551.14 | 18.09± 0.06 | AB | -- | - | - | -- | - | - | 16.34± 0.08 | B | ||
59583.20 | 18.14± 0.05 | B | -- | - | - | 17.18± 0.05 | B | -- | - | - | ||
59608.14 | 18.14± 0.06 | B | 18.55± 0.09 | B | 17.12± 0.05 | B | -- | - | - | |||
59794.38 | 18.16± 0.06 | B | -- | - | - | 17.18± 0.04 | B | -- | - | - | ||
59849.19 | 18.09± 0.06 | AB | 18.66± 0.06 | B | 17.04± 0.05 | B | -- | - | - | |||
59851.19 | 18.02± 0.05 | B | 18.66± 0.06 | B | -- | - | - | 16.28± 0.09 | B | |||
59854.19 | 18.09± 0.05 | B | -- | - | - | 17.06± 0.04 | B | 16.26± 0.08 | B | |||
59879.18 | 18.09± 0.05 | B | 18.62± 0.06 | B | 17.10± 0.06 | B | -- | - | - | |||
59903.26 | 18.23± 0.05 | B | 18.71± 0.06 | B | 17.14± 0.05 | B | 16.26± 0.08 | B | ||||
59904.15 | 18.16± 0.04 | B | 18.68± 0.04 | B | 17.14± 0.04 | B | 16.30± 0.08 | B | ||||
59932.20 | 18.20± 0.07 | AB | 18.73± 0.08 | B | 17.13± 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 [0.41 mag] | B [0.36 mag] | R [0.42 mag] | |
---|---|---|---|
B [0.41 mag] | 0.55 (21) | ||
R [0.42 mag] | 0.70 (26) | 0.63 (16) | |
I [0.29 mag] | 0.66 (17) | 0.54 (12) | 0.92 (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) | 2.39 | 0.81 | ||
R (I|R) | 3.60 | 0.64 | 2.96 | 0.04 | |
I (I|R) | 1.61 | 1.72 | 1.34 | 1.34 | 3.34 | 2.22 |
By John C. Martin, University of Illinois Springfield Henry R. Barber Research Observatory
Generated on 2023-08-14 14:15:12 UT-5