The CH4 abundance in Jupiter’s upper atmosphere | Astronomy & Astrophysics (A&A)

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Fig. A.2

Simulations using a k_g rate ten times smaller than in Table 1 and the CH₄ VMR₃ profile. The ISO measured (black) spectrum is also shown for reference. The residuals very closely resemble the hot band contribution (see red curve in Fig. 5). The 1σ noise error of the measurements is also shown.

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