Top: spectroscopic planet-to-star flux ratios with 1σ uncertainties, derived from two independent reductions of the NIRSpec/PRISM data using Eureka! and exoTEDRF, followed by the modeling of the spectroscopic secondary-eclipse lightcurves. The white lightcurve and the 196th spectroscopic lightcurve (Eureka!, both binned to 2 minute cadence for clarity) are shown along with their respective best-fit secondary-eclipse models. Bottom: planetary emission spectra, normalized to the observer’s location, derived from the planet-to-star flux ratios above and modeled PHOENIX stellar spectrum. The mean absolute difference between the two independently reduced spectra is ∼1σ, indicating excellent statistical consistency. For reference, blackbody curves corresponding to 2600, 2400, 2200, and 2000 K are also shown. The significant deviation of the planet’s spectra from blackbody expectations at shorter wavelengths is due to the dominating contribution of the reflected starlight by the planet.