Aim of the campaign
BG Indi is an F3 detached eclipsing binary system. The initial aim is to determine accurate Time of Minimum for several primary and secondary eclipses. We will repeat TOM measurements each season in order to accurately determine the period and develop an O-C diagram.
|STAR||Max V Mag||RA 2000||Krakow epoch (HJD)||BRNO period||Primary / secondary|
|Min V Mag||DEC 2000||Rozyczka et. al.*||Rozyczka et. al.* period|
*Rozyczka et. al., Mon. Not. R. Astron. Soc. 414, 2479-2485 (2011)
Note: the eclipse of the more massive component is defined as the primary eclipse in this paper, despite it being the shallower eclipse. The deeper eclipse is defined as the primary eclipse in the BRNO database. Recent data: 2455783.05767 (0.00015) TOM for primary eclipse (M. Blackford)
From Van Hamme and Manfroid, Astron. Astrophys. Suppl. Ser. 74, 247-250 (1988)
No bright field stars close enough to interfere with measurements.
The field of BG Ind is shown in the plot below.
Comparison Star Data
Please use the four comparison stars labled on the chart and catalogue values listed below.
|Comp Star||Name||RA (J2000)||DEC (J2000)||V||B-V||V-Rc|
|1||HD207964||21 55 11.34||-61 53 11.0||5.913||0.387||0.187|
|2||HD208149||21 56 14.04||-57 53 58.6||6.169||0.213||0.042|
|3||HD207575||21 52 09.67||-62 03 07.7||7.226||0.489||0.258|
|4||HD210591||22 13 05.83||-59 41 30.1||7.709||0.204||0.000|
The plot below shows a minimum observed by Mark Blackford at HJD 2455783.05767 (0.00015) as determined using PERANSO. This is 14min 12sec later than the Krakow primary eclipse prediction and 6min 15sec later than the Rozyczka et. al. secondary eclipse prediction.