2013ApJ...776L..14N

The Voyager 1 flyby of Titan in 1980 gave a first glimpse of the chemical complexity of Titan's atmosphere, detecting many new molecules with the infrared interferometer spectrometer (IRIS). These included propane (C₃H₈) and propyne (CH₃C₂H), while the intermediate-sized C₃H_xhydrocarbon (C₃H₆) was curiously absent. Using spectra from the Composite Infrared Spectrometer on Cassini, we show the first positive detection of propene (C₃H₆) in Titan's stratosphere (5σ significance), finally filling the three-decade gap in the chemical sequence. We retrieve a vertical abundance profile from 100-250 km, that varies slowly with altitude from 2.0±0.8 ppbv at 125 km, to 4.6±1.5 ppbv at 200 km. The abundance of C₃H₆ is less than both C₃H₈ and CH₃C₂H, and we remark on an emerging paradigm in Titan's hydrocarbon abundances whereby alkanes > alkynes > alkenes within the C₂H_x and C₃H_xchemical families in the lower stratosphere. More generally, there appears to be much greater ubiquity and relative abundance of triple-bonded species than double-bonded, likely due to the greater resistance of triple bonds to photolysis and chemical attack.