Table 1
Occurrence of acetylene in various astrophysical environments and objects.
| Object | Measurement technique | Investigation | Range | Ref. | ||
|---|---|---|---|---|---|---|
| Year | cm−1 | µm | ||||
| Planets | Jupiter | Cassini/CIRS mid infrared spectra | 2006 | 670 ∼ 760 | 14.9 ∼ 13.2 | (1) |
| Saturn | ISO-SWS | 1997 | 666.7 ∼ 714.3 | 15 ∼ 14 | (2) | |
| Uranus | ISO (Infrared Space Observatory) | 1998 | 694.4 ∼ 769.2 | 13 ∼ 14.4 | (3) | |
| Neptune | Voyager 2/IRIS | 1991 | 720 ∼ 740 | 13.9 ∼ 13.5 | (4) | |
| Satellites | Titan | TEXES | 2017 | 742.9 ∼ 746.7 | 13.5 ∼ 13.4 | (5) |
| Comets | Hyakutake | Infrared Telescope Facility at Mauna Kea Cryogenic echelle spectrometer (CSHELL) | 1996 | 3282 ∼ 3288 | 3.047 ∼ 3.041 | (6) |
| Carbon stars | IRC +10216 | TEXES | 2008 | 714.29 ∼ 909.09 | 14 ∼ 11 | (7) |
| Orion IRc2 | SOFIA/EXES | 2018 | 750.19 ∼ 771.60 | 13.33 ∼ 12.96 | (8) | |
Notes. The table summarizes the detection of C2H2 across different objects, including planets, satellites, comets, carbon stars, and the Orion IRc2. Columns provide details on the object type, measurement technique used (e.g., ISO-SWS, TEXES, SOFIA/EXES), year of investigation, spectral range in wavenumber (cm−1) and wavelength (µm), and the corresponding references. These data highlight the widespread presence of acetylene and the variety of observational tools employed to study it in diverse cosmic settings (Pentsak et al. 2024). Among these, we focus on the frequency ranges exhibiting infrared activity in various acetylene observational data. References: (1) Nixon et al. (2007); (2) de Graauw et al. (1997); (3) Encrenaz et al. (1998); (4) Bézard et al. (1991); (5) Bézard et al. (2022); (6) Brooke et al. (1996); (7) Fonfría et al. (2008); (8) Rangwala et al. (2018).
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