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$\begin{figure} \includegraphics[width=10.8cm,clip]{Fi302_f1.eps} \end{figure}$ Figure 1: The calibrated spectrum of Uranus (black line). Red line: best fit model, including CO fluorescence, H₃⁺ emission, and tropospheric emission (see text). Green line: three-component model with CO fluorescence replaced by CO thermal emission at 150 K, normalized at 4.71 $\mu$ m.
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In the text

$\begin{figure} \includegraphics[width=10.8cm]{Fi302_f2.eps} \end{figure}$ Figure 2: The raw (undivided) spectrum of Uranus (black line) compared to different synthetic models multiplied by the atmospheric transmission function (see text). Red line: best-fit model (CO = PH₃ = 0); green line: CO = $2.0\times 10^{-8}$ , PH₃ = 0; blue line: PH $_3 = 1.0\times 10^{-6}$ , CO = 0.
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In the text

$\begin{figure} \includegraphics[width=10.8cm,clip]{Fi302_f1.eps} \end{figure}$	Figure 1: The calibrated spectrum of Uranus (black line). Red line: best fit model, including CO fluorescence, H₃⁺ emission, and tropospheric emission (see text). Green line: three-component model with CO fluorescence replaced by CO thermal emission at 150 K, normalized at 4.71 $\mu$ m.
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$\begin{figure} \includegraphics[width=10.8cm]{Fi302_f2.eps} \end{figure}$	Figure 2: The raw (undivided) spectrum of Uranus (black line) compared to different synthetic models multiplied by the atmospheric transmission function (see text). Red line: best-fit model (CO = PH₃ = 0); green line: CO = $2.0\times 10^{-8}$ , PH₃ = 0; blue line: PH $_3 = 1.0\times 10^{-6}$ , CO = 0.
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