Geometric albedo of WASP-12 b and WASP-76 b in the CHEOPS and TESS bandpasses (Corrigendum) (Astronomy and Astrophysics (2024) 684 (A27) DOI: 10.1051/0004-6361/202348270)

This is a corrigendum to Akinsanmi et al. (2024) andDemangeon et al. (2024). The retrieval code used in these worksomitted a factor of λ in the integration of the stellar (F⋆) andplanetary emission (Fp) necessary to obtain the planet-to-starflux ratio (Fd/F⋆) at each observing band of the atmosphericretrievals (see, for example, Eq. (13) of Akinsanmi et al. 2024).The λ factor is needed because the passband response functions (Tinst) are photon counters. The corrected calculation ofthe thermal planet-to-star flux ratio is (Formula presented) where Rp and R⋆ are the planet and star radii. However, we note that the general analysis, results, and conclusions of the articles are not affected by this error. The omission of the λ factors is only relevant for broad bands and when the emission spectra vary significantly over the bands. This means that in our analyses, only the CHEOPS (CHaracterisingExOPlanet Satellite, Benz et al. 2021) and TESS (TransitingExoplanet Survey Satellite, Ricker et al. 2015) bands were significantly affected. The revised values, tables, and figures aregiven below. 1. WASP-12 b In Akinsanmi et al. (2024), the atmospheric retrievals only included infrared eclipse observations as constraints (Sect. 5.2.1). Thus, the retrieval results were not affected in a statistically significant manner. We confirmed this by re-running the analysis with the corrected passband calculation. The thermal contributions inferred from the retrieval to the eclipse depths in the CHEOPS and TESS passbands are revised from 205 ± 10 and 480 ± 19 ppm (Sect. 5.3) to 270 ± 11 and 511 ± 18 ppm, respectively. This led to updated geometric albedos, from Ag = 0.083 ± 0.015 and 0.010 ± 0.023 to Ag = 0.042 ± 0.018 and −0.010 ± 0.024 in the CHEOPS and TESS bands, respectively. This correction does not alter our general conclusion that WASP-12 b has a low geometric albedo, which is consistent with the low reflectivity observed in other ultra-hot Jupiters. 2. WASP-76 b Similarly to what was done for WASP-12 b, the atmospheric retrievals of WASP-76 b performed in Demangeon et al. (2024) only included the infrared eclipse observations as constraints (Sect. 5.1.1). The retrieval results were thus not affected in a statistically significant manner. The retrieval-inferred thermaleclipse depths over the CHEOPS and TESS bands have increased (Table presented) (Figure presented) from their original values. Figure 1 shows the corrected bandintegrated eclipse depths inferred from each retrieval model (correction of the insets in Figs. 4 and C1 of Demangeon et al. 2024). Table 1 shows the corrected geometric albedos (correction of Table 3 of Demangeon et al. 2024). This correction (lower geometric albedo values) does not change the conclusions (Sect. 6.1 of Demangeon et al. 2024), that WASP-76b has a low geometric albedo, consistent with that of other ultra-hot Jupiters. Taking the different composition hypotheses and the different reductions of the infrared datasets into account, we can set a 1- sigma upper limit of 0.13 and 0.19 in the CHEOPS and TESS bandpasses, respectively (correction of the values provided in Table 6).