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This is a difficult exoplanet to observe because it's a double star with separation = 11"arc. You need really good seeing for use of a photometry aperture that restricts flux measurements to just the exoplanet star (~0.5 mag fainter). It's OK to include both stars in your photometry aperture, but please note that this was done in a header comment line.
Basic Data - Updated 2009.09.22
RA = 22:57:46.8, Decl = +38:40:30
Season = September 09
V ~ 10.2, B-V = 0.7; B~10.9, V~10.2, R~9.81, I ~ 9.56 (for combined flux of stars A and B: B~9.8, V~9.1, R~8.77, I = 8.52)
HJDo = 4363.94656 (72), Johnson et al, 2008 & P = 4.4652934 (93) day, Johnson et al, 2008 (as listed in Schneider's Extrasolar Planets Encyclopedia)
HJDo = 4363.9463 (7) & P = 4.4653194 (13) from fit to data in AXA
Depth = 13.0 ± 1.5 mmag if only the exoplanet star is measured, and 6.0 ± 1.5 if both stars are measured. Winn et al, 2007 report 14.0 ± 0.5 mmag (z-band).
Length = 2.67 ± 0.2 (C & R-band), 2.65 ± 0.02 hr (z-band), Winn et al, 2007
Fp = 0.44 ± 0.05, F2 = 0.81 ± 0.15
b = 0.70
of Transit Light Curves - Updated
Transit Light Curves
9816SG2 The small depth probably is due to the photometry aperture including both components A nd B (see finder image below).
Came early, whereas a week earlier it came late..
Transit was late. Depth is lower than for R-band, probably because CLR filter is bluer than R (& limb darkening will produce lower depth at bluer bands if exoplanet transit chord is close to star center). Length agrees. Good job for a 12-inch and using 10-second exposure times (with associated low duty cycle).
Johnson, JOhn Asher et al, "Measurement of the Spin-Orbit Angle of Exoplanet
HAT-P-1b", arXiv:0806.1734vJ, http://adsabs.harvard.edu/abs/2008arXiv0806.1734J
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L. Gary. Nothing on this web page is copyrighted. This site opened: September 08, 2007. Last Update: 2009.09.26