Possible explanation for the asymmetry of our detection. a) panel, the asymmetry could be due to the eastward shift of the hotspot. During the pre-eclipse phase (when we observe the eastern side with the hotspot), the observed temperature gradient is shallower. The temperature gradient is steeper during the post-eclipse phase (when we observe more of the western side). As a result, the spectral line contrast (linked to these gradients) will be weaker before the eclipse and stronger after the eclipse. b) panel, the fainter detection during pre-eclipse compared to post-eclipse observations could be due to the presence of clouds and the associated glory effect in the eastern hemisphere, a hint of this could be the hotspot offset detected in the optical CHEOPS and TESS light curves.