Image Details
Caption: Figure A5.
Comparison of the phase-resolved emission spectra for the Eureka! data reduction (v1) and the exoTEDRF + Eureka! reduction (v2). All pairs of primary and secondary spectra agree well (﹩{\chi }_{\nu }^{2}\lt 1﹩), with the nightside flux showing signs of possible biasing due to the required use of Eureka!’s force_positivity feature, forcing nonnegative flux, as discussed in Section 2.4.
© 2026. The Author(s). Published by the American Astronomical Society.