Table 3
Best-fit planet system parameters from χ2 optimization and confidence intervals from MCMC sampling of the posterior parameter distributions for the Run 1 white light curve of HAT-P-32Ab.
| Parameter | This work | Hartman et al. (2011, e ≡ 0 | Gibson et al. (2013b) | Seeliger et al. (2014) | |
| filter/range | 518−918 nm | I, z, g | 520.6−932.5 nm | rS, RB, RC, Clear | |
|
|
|||||
| Rp/R⋆ |
|
|
|
|
|
| ap/R⋆ |
|
|
|
|
|
| i |
|
|
|
|
|
| P [d] |  (fixed) |
|
 (fixed) |
|
|
| TC1 − 2 456 185 [BJDUTC] |
|
 a
|
a
|
 a
|
|
| e |  (fixed) |
(fixed) |
(fixed) |
(fixed) |
|
| u1 |
|
|
|
|
|
| u 2 |
|
|
|
|
|
| TC2 − 2 456 200 [BJDUTC] a |
|
|
|
|
|
Notes. The red noise factor used to inflate the error bars of our results is β = 1.345. For comparison the planet parameters obtained from three recent works (Hartman et al. 2011, e ≡ 0; Gibson et al. 2013b; Seeliger et al. 2014) are listed.
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