Erratum for: A&A 669, A3 (2023), https://doi.org/10.1051/0004-6361/202243240

In Appendix B of the original article we investigated the sensitivity of JWST/MIRI for the filters F1000W and F2100W. We transformed sensitivities valid for an unresolved point source into surface brightness sensitivities using Eq. (12) from Glasse et al. (2015). For the filter F1000W, the resulting detection limit is given in the original article as ≈4.2 × 10⁻⁵ Jy arcsec⁻². This limit should have been read ≈3.5 × 10⁻⁶ Jy arcsec⁻². This is only a typographical error, and the correct value was used for the analysis. For the filter F2100W, the resulting detection limit is given in the original article as ≈4.2 × 10⁻⁴ Jy arcsec⁻². However, in our analysis, a limit of ≈3.5 × 10⁻⁵ Jy arcsec⁻² was used. This value was erroneously calculated; the correct limit is ≈7.9 × 10⁻⁶ Jy arcsec⁻². This detection limit is lower than the used limit, and hence the performance of JWST/MIRI at a wavelength of 21 µm was underestimated.

Consequently, the exposure times required to detect structures in the surface brightness distributions using JWST/MIRI at 21 µm are shorter than what is given in the original article. To detect intermediate surface brightness values of 5 × 10⁻⁵ Jy arcsec⁻² with a SNR of 3 an exposure time of t_exp ≈ 2.5 min is required (instead of the t_exp ≈ 10 min given in the original article).

The third panel of Fig. B.2 shows horizontal lines with too high sensitivity limits. This is corrected here in Fig. 1. Using the correct sensitivity limits, an exposure time of t_exp = 1 h is sufficient to detect emission with surface brightness values corresponding to isophotes with semimajor axes of up to a ~ 190 au–220 au with a S/N of 3. With t_exp = 5 h, all halo regions investigated can be detected with a S/N of at least 3.

The red contour lines in Figs. B.3 and B.4 are valid for an exposure time of t_exp ≈ 14 min (instead of the t_exp = 1 h given in the original article). For the system n-i-M4, an exposure time of t_exp ≳ 2 h would be required to significantly detect the spiral pattern (instead of the t_exp ≳ 8 h given in the original article).

The error only affects the conclusions about the feasibility of detecting certain disk features with JWST/MIRI at a wave-length of 21 µm: a shorter exposure time than what is stated in the original article is required. The main conclusions of the original article remain unchanged.

Fig. 1 Same as the third panel of Fig. B.2 in the original article, but with the correct sensitivity limits used to compute the surface brightness values of the horizontal dashed lines. These horizontal lines denote the minimum surface brightness required to achieve a certain detection significance (S/N) using JWST/MIRI at a wavelength of 21 µm. Red lines are for an exposure time of texp = 1 h, blue lines for texp = 5 h.

References

© The Authors 2024

All Figures

Fig. 1 Same as the third panel of Fig. B.2 in the original article, but with the correct sensitivity limits used to compute the surface brightness values of the horizontal dashed lines. These horizontal lines denote the minimum surface brightness required to achieve a certain detection significance (S/N) using JWST/MIRI at a wavelength of 21 µm. Red lines are for an exposure time of texp = 1 h, blue lines for texp = 5 h.

In the text