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Home All issues Volume 700 (August 2025) A&A, 700 (2025) C1 Full HTML
Issue
A&A
Volume 700, August 2025
Article Number C1
Number of page(s) 3
Section Planets, planetary systems, and small bodies
DOI https://doi.org/10.1051/0004-6361/202556327e
Published online 31 July 2025

Erratum for: A&A, 684, A27 (2024), https://doi.org/10.1051/0004-6361/202348270

Erratum for: A&A, 685, A63 (2024), https://doi.org/10.1051/0004-6361/202348502

This is a corrigendum to Akinsanmi et al. (2024) and Demangeon et al. (2024). The retrieval code used in these works omitted a factor of λ in the integration of the stellar (F⋆$\mathcal{F}_{\star}$) and planetary emission (Fp$\mathcal{F}_{\mathrm{p}}$) necessary to obtain the planet-to-star flux ratio (Fd/F*) at each observing band of the atmospheric retrievals (see, for example, Eq. (13) of Akinsanmi et al. 2024). The λ factor is needed because the passband response functions (Tinst$\mathcal{T}_{\text {inst}}$) are photon counters. The corrected calculation of the thermal planet-to-star flux ratio is FdF⋆=(RpR⋆)2∫Fp(λ)Tinst(λ)λdλ∫F⋆(λ)Tinst(λ)λdλ,$\frac{F_{\mathrm{d}}}{F_{\star}}=\left(\frac{R_{\mathrm{p}}}{R_{\star}}\right)^{2} \frac{\int \mathcal{F}_{\mathrm{p}}(\lambda) \mathcal{T}_{\text {inst}}(\lambda) \lambda \mathrm{d} \lambda}{\int \mathcal{F}_{\star}(\lambda) \mathcal{T}_{\text {inst}}(\lambda) \lambda \mathrm{d} \lambda},$(1) 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 (CHaracterising ExOPlanet Satellite, Benz et al. 2021) and TESS (Transiting Exoplanet Survey Satellite, Ricker et al. 2015) bands were significantly affected. The revised values, tables, and figures are given 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 thermal eclipse depths over the CHEOPS and TESS bands have increased from their original values. Figure 1 shows the corrected band-integrated 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).

Table 1.

WASP-76b’s Ag estimates.

thumbnail Fig. 1

Corrected reproduction of the insets of Figs. 4 and C1 of Demangeon et al. (2024): WASP-76 b occultation atmospheric retrievals for a model including the TiO and VO optical absorbers (left panel), including only VO (middle), and excluding both TiO and VO (right). The light blue, dark blue, and orange curves and their associated shaded areas show the retrieved spectra and 68% credible intervals when fitting the D1, D2, and D3 occultation observations, respectively (see the legend and notes in Table 1). The grey markers show the CHEOPS and TESS occultation measurements, although the fits are not constrained by these observations. The coloured square markers show the corrected model eclipse-depths integrated over the CHEOPS and TESS bands (see the passband response functions in grey at the bottom of the panels).

References

  1. Akinsanmi, B., Barros, S. C. C., Lendl, M., et al. 2024, A&A, 685, A63 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
  2. Benz, W., Broeg, C., Fortier, A., et al. 2021, Exp. Ast., 51, 109 [Google Scholar]
  3. Demangeon, O. D. S., Cubillos, P. E., Singh, V., et al. 2024, A&A, 684, A27 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
  4. Edwards, B., Changeat, Q., Baeyens, R., et al. 2020, AJ, 160, 8 [Google Scholar]
  5. Fu, G., Deming, D., Lothringer, J., et al. 2021, AJ, 162, 108 [NASA ADS] [CrossRef] [Google Scholar]
  6. Ricker, G. R., Winn, J. N., Vanderspek, R., et al. 2015, J. Astron. Teles. Instrum. Syst., 1, 014003 [Google Scholar]

© The Authors 2025

Licence Creative CommonsOpen Access article, published by EDP Sciences, under the terms of the Creative Commons Attribution License (https://creativecommons.org/licenses/by/4.0), which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited.

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All Tables

Table 1.

WASP-76b’s Ag estimates.

In the text

All Figures

thumbnail Fig. 1

Corrected reproduction of the insets of Figs. 4 and C1 of Demangeon et al. (2024): WASP-76 b occultation atmospheric retrievals for a model including the TiO and VO optical absorbers (left panel), including only VO (middle), and excluding both TiO and VO (right). The light blue, dark blue, and orange curves and their associated shaded areas show the retrieved spectra and 68% credible intervals when fitting the D1, D2, and D3 occultation observations, respectively (see the legend and notes in Table 1). The grey markers show the CHEOPS and TESS occultation measurements, although the fits are not constrained by these observations. The coloured square markers show the corrected model eclipse-depths integrated over the CHEOPS and TESS bands (see the passband response functions in grey at the bottom of the panels).
In the text

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