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Description
The ultra-hot Jupiter WASP-33b shows evidence for a thermal inversion in the form of emission lines of atoms and molecules, including OH and Fe. Phase-curve measurements at optical wavelengths with TESS show a westward phase-offset while observations in the infrared with the Spitzer Space Telescope show an Eastward offset. We obtained phase-curve observations at high-spectral resolution at optical wavelengths with Subaru/HDS as well as CFHT/ESPaDOnS.
Using log-likelihood mapping and integrating a simple phase-curve model we demonstrate that it is possible to measure phase-curve variations, although unequal pre/post eclipse sampling can result in biases. For the Fe I emission, we show evidence that the peak is after eclipse at +22 +/- 12 degrees, consistent with the optical phase-curve. We also constrain the day-night contrast to be >0.9, indicating that, in the case of Fe I, the nightside contributes less than 10% of the day-side flux in our simple model.
