Reproduction package for Spectroscopically resolved partial phase curve of the rapid heating and cooling of the highly-eccentric Hot Jupiter HAT-P-2b with WFC3

This is a basic reproduction package for the paper "Spectroscopically resolved partial phase curve of the rapid heating and cooling of the highly-eccentric Hot Jupiter HAT-P-2b with WFC3" by [Jacobs, B.; Désert, J. -M.; Lewis, N. et al. (2024)] Abstract: The extreme environments of transiting close-in exoplanets in highly-eccentric orbits serve as ideal laboratories for testing exo-atmospheric physics. Spectroscopically resolved phase curves not only allow for the characterization of their thermal response to irradiation changes but also unveil phase-dependent atmospheric chemistry and dynamics. We observed a partial phase curve of the highly-eccentric close-in giant planet HAT-P-2b (e = 0.51023) with the Wide Field Camera 3 (WFC3) aboard the Hubble Space Telescope. Using these data, we update the planet’s orbital parameters and radius, and we retrieve high-frequency pulsations consistent with those reported in Spitzer data. We find that the peak in planetary flux occurs at 6.7 ± 0.6 hr after periastron, with a heating timescale of 9.0+3.5 −2.1 hr, and a cooling timescale of 3.6+0.7−0.6 hr. We compare the light-curve to a suite of 1-dimensional and 3-dimensional forward models, varying the planet’s chemical composition. The strong contrast in flux increase and decrease timescales before and after periapse indicates an opacity term that emerges during the planet’s heating phase. We suggest that more emerging H− than expected from chemical equilibrium models could be the reason for the mismatch between models and the data. We used a common-mode based method that does not assume a functional form to extract phase-resolved spectra. The analysis of these spectra is challenging because of the unknown accuracy of the spectral slope and absolute flux levels. The phase-resolved spectra are largely featureless, possibly indicating an inhomogeneous dayside. However, we identified an anomalously high flux in the spectroscopic bin that coincides with the hydrogen Paschen β line and that is potentially connected to the planet’s orbit. We exclude an instrumental origin and we discuss several alternative, astrophysical origins.