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This article has an erratum: [https://doi.org/10.1051/0004-6361/202038753e]


Table 3

Spectroscopic and photometric datasets used for the bolometric flux computation with the corresponding spectral ranges.

Target INES TD1 Adelman (+) Visible 2MASS fbol [erg cm−2 s−1] fbol [erg cm−2 s−1]
spectra This work from modelling
HD 4778 [1265 ... 3180] Y [3900 ... 6800] (a) J, H, K 0.97 ± 0.10 ×10−7
HD 108662 [1265 ... 3180] [3300 ... 7100] [4000 ... 6800] (a) J, H, K 2.24 ± 0.21× 10−7 (•) 2.53 ± 0.15 × 10−7
HD 108945 [1265 ... 3180] Y [3300 ... 7100] [3900 ... 6800] (a) J, H, K 1.68 ± 0.15 × 10−7
HD 120198 [1265 ... 3180] Y [3300 ... 7100] [3725 ... 7210] (b) J, H, K 1.62 ± 0.13 × 10−7
HD 153882 Y [3390 ... 7850] [3535 ... 7405](c) J, H, K 0.81 ± 0.06× 10−7 0.79 ± 0.04 × 10−7
HD 188041 [1977 ... 3180] Y [3390 ... 7850] [3535 ... 7405] (c) J, H, K 1.34 ± 0.16 × 10−7 1.34 ± 0.25 ×10−7
HD 204411 Y [3300 ... 6800] [3720 ... 7215] (b) J, H, K 1.90 ± 0.15× 10−7 1.84 ± 0.15 ×10−7
HD 220825 [3300 ... 7850] [3725 ... 7215] (b) J, H, K 2.30 ± 0.17 ×10−7

Notes. The bolometric fluxes obtained from our work and from self-consistent atmosphere modelling are given in the last two columns. See text for details. (+) Adelman data are photometric values collected over the optical range. Visible spectra: (a) ELODIE; (b) OAN; (c) MILES. (∙) We accounted for the 1.32 scale factor of the IUE flux, as explained in Sect. 3.1.

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