2020ApJ...903L..22T

Titan harbors a dense, organic-rich atmosphere primarily composed of N₂ and CH₄, with lesser amounts of hydrocarbons and nitrogen-bearing species. As a result of high-sensitivity observations by the Atacama Large Millimeter/submillimeter Array (ALMA) in Band 6 (∼230-272 GHz), we obtained the first spectroscopic detection of CH₃C₃N (methylcyanoacetylene or cyanopropyne) in Titan's atmosphere through the observation of seven transitions in the J=64→63 and J=62→61 rotational bands. The presence of CH₃C₃N on Titan was suggested by the Cassini Ion and Neutral Mass Spectrometer detection of its protonated form: C₄H₃NH⁺, but the atmospheric abundance of the associated (deprotonated) neutral product is not well constrained due to the lack of appropriate laboratory reaction data. Here, we derive the column density of CH₃C₃N to be (3.8-5.7) x 10¹² cm^–2 based on radiative transfer models sensitive to altitudes above 400 km Titan's middle atmosphere. When compared with laboratory and photochemical model results, the detection of methylcyanoacetylene provides important constraints for the determination of the associated production pathways (such as those involving CN, CCN, and hydrocarbons), and reaction rate coefficients. These results also further demonstrate the importance of ALMA and (sub)millimeter spectroscopy for future investigations of Titan's organic inventory and atmospheric chemistry, as CH₃C₃N marks the heaviest polar molecule detected spectroscopically in Titan's atmosphere to date.