Dayside reflection and emission brightness contributions. Left: geometric albedo (A_g) as a function of the dayside brightness temperature for the estimated occultation depths in CHEOPS (blue) and TESS (red). The decreasing intensity of the colour shades corresponds to the 1 σ, 2 σ, and 3 σ uncertainties in the computation of A_g for each T_day. The overlapping region provides the true constraints on the two parameters represented by the posterior distribution in grey. The individual posteriors of (A_g) and (T_day) are presented in the side panels. The resultant values are reported in the text. Subpanel: reflection and emission contributions to the occultation depth of the CHEOPS and TESS passbands. The identical height of the reflection component reflects the assumption of α = 1. Right: Kurucz stellar model [T_eff = 9000, [Fe/H] = 0 and log = 4.5] along with the CHEOPS and TESS passband responses. The dayside planetary black-body flux (×100) is also plotted for a comparison with the stellar flux. T_day = 2600 K.