Table 2
Summary of literature and derived planet properties for HR 8799 c.
Planet | Ref. | Clouds | M (MJup) | log g (cgs) | Teff (K) | R (RJup) | [M/H] | C/O | log Lbol/L⊙ |
---|---|---|---|---|---|---|---|---|---|
c | C11 | Thick | 7–17.5 | 4–4.5 | 1000–1200 | … | 0 | … | −4.7 ± 0.1 |
G11 | Slab | 1.1 | 3.5 | 1200 | 0.97 | … | … | −4.7 ± 0.1 | |
M11 | Power law | 3–11 | 4.0–4.3 | 950–1025 | … | … | … | −4.7 ± 0.1 | |
M12 | AM01 | 8–11 | 4.1 ± 0.1 | 950 ± 60 | 1.32–1.39 | 0 | … | −4.90 ± 0.1 | |
K13 | … | 3–7 | 3.5–4.0 | 1100 ± 100 | 1–1.5 | … | 0.65 ± 0.1 | … | |
B16 | ER4 | … | 3.8–3.9 | 1200 | 1.0 | 0.5 | … | … | |
L17 | Mie | … | 4.5 ± 0.1 | 960 ± 20(a) | 1.25 ± 0.02 | … | 0.55 ± 0.01 | … | |
G18 | Various | … | 3.5–4.0 | 1100–1350 | 0.7–1.2 | … | … | −4.58 to −4.82 | |
W20 | Deck | … | ![]() |
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1.47 ± 0.02 | … | ![]() |
−4.59 ± 0.004 | |
W20(b) | Deck | … | ![]() |
1102 ± 2 | 1.20 | … | ![]() |
−4.69 ± 0.0002 | |
W21(c) | BT-Settl | … | ![]() |
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… | … | … | … | |
R21(d) | Slab | … | ![]() |
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… | 0 | ![]() |
… | |
W23 | AM01 | … | ![]() |
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… | |
Best A ∩ B | AM01 | ![]() |
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BMA A ∩ B | AM01 | ![]() |
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A ∩ B | AM01 | ![]() |
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Grids | Various | 1.24–10.3 | 3.5–4.5 | 1100–1200 | 0.8–1.31 | > 1.0 | 0.3–0.8 | −4.65 to −4.72 |
Notes. (a) Only Tint, a model parameter, is reported. (b) W20 compared using strong and weak radius priors to enforce physicality. (c) W21 used high resolution spectroscopy, and did not infer masses or radii, using masses of 7.2 ± 0.7 MJup for the inner three planets and 5.8 ± 0.5 MJup for HR 8799 b. A radius of 1.2 ± 0.1 RJup was used for all planets. (d) R21 uncertainties were limited by the coarseness and boundaries of their model grid.(e) W23 report the temperature at 3.3 bar rather than the effective temperature.(f) The metallicity of W23 was found by averaging the retrieved C/H and O/H ratios.
References. C11: Currie et al. (2011); G11: Galicher et al. (2011); M11: Madhusudhan et al. (2011); M12: Marley et al. (2012); L13: Lee et al. (2013); K13: Konopacky et al. (2013); B16: Bonnefoy et al. (2016); L17: Lavie et al. (2017); G18: Greenbaum et al. (2018); W20: Wang et al. (2020b); W21: Wang et al. (2021b); R21: Ruffio et al. (2021); W23:Wang et al. (2023).
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