Table 1
Parameters adopted in our optical and NIR phase curve simulations of WASP-12 b.
| Parameter | Description | Optical/TESS(†) | NIR/PRISM(‡) |
|---|---|---|---|
| Rp (R*) | Scaled spherical radius | 0.1160 | 0.1168 |
| Rv (R*) | Scaled volumetric radius(◊) | 0.1222 | 0.1232 |
| a/R* | Scaled semimajor axis | 3.061 | 3.061 |
| b | Impact parameter | 0.344 | 0.344 |
| cLD | Power-2 LDCs(§) | 0.6371 | 0.2862 |
| αLD | 0.6175 | 0.4183 | |
| Fd/F* (ppm) | Dayside flux | 466 | 3306 |
| Fn/F* (ppm) | Nightside flux | 0 | 500 |
| δ (°) | Phase offset | 6.2 | 20 |
| AEV (ppm) | EV semi-amplitude | 65 | 60 |
| ADB (ppm) | DB semi-amplitude | 2.34 | 1.18 |
| h2f | Love number(◊) | 1.565 | |
| QM | Planet-to-star mass ratio(◊) | 0.00098 | |
Notes.(†) The TESS parameter values are the derived values from the analysis of four sectors of WASP-12 TESS observations Wong et al. (2022).(§) These values were obtained using LDTk (Parviainen 2018) in the different passbands.(‡) Values for the PRISM parameters Rp and Fd/F*, are obtained by integrating the modeled transmission (Stevenson et al. 2014) and emission spectra (Hooton et al. 2019) across the PRISM wavelength range, AEV and ADB are estimated using Eqs. (6) and (8), respectively, while δ is the derived value from the 2013 Spitzer 4.5 µm phase curve of WASP-12b (Bell et al. 2019).(◊) These parameters are specific to the ellipsoidal planet model where we assume the same h2f as Jupiter, Rv is the volumetric radius that produces the same transit depth as the spherical planet of radius Rp , and QM is taken from Collins et al. (2017).
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