Table 1
Summary of the different haze analogs produced with the PAMPRE and COSmIC setups using different gas compositions.
| Analog | Gas composition | Setup | Production a (hours) | Measurements b | Spectral range |
|---|---|---|---|---|---|
| Titan 1 | 90% N2–10% CH4 | PAMPRE | 3 | TS, RE, FTIRS | 0.3–200 μm |
| COSmIC | 8.5 | RS, RE, FTIRS | 0.4–200 μm | ||
| Titan 2 | 95% N2–5% CH4 | PAMPRE | 3 | TS, RE, FTIRS(*) | 0.3–200 μm |
| COSmIC | 10 | RS, RE, FTIRS(*) | 0.4–200 μm | ||
| Pluto | 95% N2–4.95% CH4–0.05% CO | PAMPRE | 3 | TS, FTIRS | 0.27–200 μm |
| COSmIC | 11 | RS, RE, FTIRS(*) | 0.4–200 μm | ||
| Exoplanet 1 | 95% N2–4% CH4–1% CO | PAMPRE | 5 | TS, FTIRS | 0.285–200 μm |
| COSmIC | 18 | RS, FTIRS | 0.35–30 μm | ||
| Exoplanet 2 | 95% Ar–5% CH4 | PAMPRE | 5 | TS, RE, FTIRS(*) | 0.3–200 μm |
| COSmIC | 18 | RS, RE, FTIRS | 0.4–15 μm | ||
| Exoplanet 3 | 95% Ar–4% CH4−1% CO | PAMPRE | 7 | TS, FTIRS | 0.25–200 μm |
| COSmIC | 18 | RS, FTIRS | 0.3–12 μm |
Notes. a The production refers to the duration of the experiment. b The following measurements were carried out to determine refractive indices from UV to NIR: transmission spectroscopy (TS), reflection spectroscopy (RS), and reflection ellipsometry (RE). Fourier-transform IR spectroscopy (FTIRS) was used to obtain refractive indices from NIR to FIR. The FTIRS measurements were also used to characterize the MIR absorption properties of haze analogs at low temperatures (40–288 K, see Section 3.4). These low-temperature measurements were performed on a few analogs here marked with (*).
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