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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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