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Table 5

Comparison of WASP-7 b parameters with those of other hot and ultra-hot Jupiters.

Planet Teq (K) H(a) (km) ΔA (10−3) D2 line contrast (%) D2 FWHM (Å) D1 line contrast (%) D1 FWHM (Å) Refs.(d)
WASP-76 b 2160 1479 0.23 0.37 ± 0.09 0.61 ± 0.17 0.50 ± 0.08 0.68 ± 0.12 1, A
WASP-121 b 2358 1011 0.26 0.69 ± 0.12 0.73 ± 0.09 0.25 ± 0.09 0.9 ± 0.1 2, B
WASP-21 b 1333 951 0.25 0.31 ± 0.05 3, C
WASP-52 b 1315 672 0.4 1.31 ± 0.13 0.42 ± 0.03 1.09 ± 0.16 0.22 ± 0.03 4, D

WASP-7 b 1530 383 0.07 0.50 ± 0.06 0.13 ± 0.02 0.13 ± 0.04 0.13 ± 0.02 5,E
WASP-7 b (alt)(c) 0.49 ± 0.05 0.17 ± 0.02 0.19 ± 0.03 0.17 ± 0.02 5,E

MASCARA-2 b 2260 315 0.06 0.29 ± 0.04 0.16 ± 0.02 0.29 ± 0.04 0.15 ± 0.02 6, F
HD 189733 b 1140 200 0.11 0.64 ± 0.07 0.52 ± 0.08 0.40 ± 0.07 0.52 ± 0.08 7, G

Notes. (a) Atmospheric scale height. (b) Fraction of the stellar disk covered by an atmospheric annulus with a height of one scale height. (c) For WASP-7 b we show the result of the modeling by considering all spectra and by ignoring ten post-transit spectra (alt). (d) The numerals specify references for Na i D line contrasts and FWHMs, and letters denote references for the planetary effective temperature. We calculated the scale heights based on the references.

References. (1) Seidel et al. (2019); (A) West et al. (2016); (2) Cabot et al. (2020); (B) Delrez et al. (2016); (3) Chen et al. (2020a); (C) Ciceri et al. (2013); (4) Chen et al. (2020b); (D) Hébrard et al. (2013); (5) this work; (E) Southworth (2012); (6) Casasayas-Barris et al. (2019); (F) Talens et al. (2018); (7, G) Wyttenbach et al. (2015).

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