Table A.1
Film thicknesses derived for each PAMPRE analog sample from UV to near-IR using the transmission data.
| PAMPRE analog | Gas composition | Spectral range | Position | Film thickness a (nm) |
|---|---|---|---|---|
| Titan 1 | 90% N2−10% CH4 | 0.3-2.5 μm | 1 | 1737.0 ± 12.0 |
| 2 | 1745.2 ± 11.7 | |||
| 3 | 1740.2 ± 13.0 | |||
| Titan 2 | 95% N2–5% CH4 | 0.3-2.5 μm | 1 | 1572.2 ± 11.3 |
| 2 | 1672.6 ± 25.1 | |||
| Pluto | 95% N2–4.95% CH4−0.05% CO | 0.27-2.5 μm | 1 | 1183.9 ± 15.4 |
| 2 | 1184.9 ± 20.1 | |||
| Exoplanet 1 | 95% N2–4% CH4–1% CO | 0.285-2.5 μm | 1 | 1670.2 ± 13.4 |
| 2 | 1672.6 ± 12.5 | |||
| 3 | 1676.7 ± 13.6 | |||
| Exoplanet 2 | 95% Ar–5% CH4 | 0.3-2.5 μm | 1 | 606.0 |
| 2 | 606.6 | |||
| 3 | 607.9 | |||
| Exoplanet 3 | 95% Ar–4% CH4−1% CO | 0.25-2.5 μm | 1 | 1008.7 ± 16.1 |
| 2 | 1009.3 ± 13.8 |
Notes. a With the Swanepoel method, a thickness value can be derived for each adjacent interference fringe. An uncertainty can thereby be obtained using the different pairs of fringes observed in the spectrum. The error given here corresponds to the maximum deviation from the mean value of the thickness.
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