Infrared Emission of Polycyclic Aromatic Hydrocarbon Molecules in Titan: Cyanonaphthalenes

Abstract As the only moon in the solar system with a thick atmosphere, Titan is a compelling and enigmatic world containing a complex organic haze. Polycyclic aromatic hydrocarbon (PAH) molecules are believed to play an essential role in the formation of Titan’s aerosols and haze layers. The existence of PAHs in Titan’s upper atmosphere has been revealed by the detection of the 3.28 μm emission band with Cassini’s Visual and Infrared Mapping Spectrometer (VIMS). However, there is little knowledge about the identity, composition, size and abundance of PAH molecules in Titan’s atmosphere. Due to its unprecedented sensitivity and spectral coverage and resolution, the advent of the James Webb Space Telescope (JWST) could possibly enable a full characterization of the chemical makeups of Titan’s aerosols. In particular, with a much better spectral resolution than Cassini’s VIMS, JWST’s Near Infrared Spectrograph (and Mid-Infrared Instrument) could enable the spectral bands to be better resolved, potentially providing crucial information about which PAHs are really present in Titan’s upper atmosphere. To facilitate JWST to search for and identify Titan’s PAH molecules, we are performing a systematic study of the photophysics of PAHs in Titan’s upper atmosphere. As a pilot study, here we report the infrared emission spectra of vibrationally excited cyanonapthalenes and their ions which are composed of two fused benzene rings and one nitrile (–CN) group. The calculated emission spectra will help JWST to quantitatively determine or place an upper limit on the abundances of cyanonapthalenes in Titan’s upper atmosphere.