2016MNRAS.460.2648P

The understanding of organic content of protoplanetary discs is one of the main goals of the planet formation studies. As an attempt to guide the observational searches for weak lines of complex species in discs, we modelled the (sub)millimetre spectrum of gaseous methanol (CH_3OH), one of the simplest organic molecules, in the representative T Tauri system. We used 1+1D disc physical model coupled to the gas-grain alchemic chemical model with and without 2D-turbulent mixing. The computed CH_3OH abundances along with the CH_3OH scheme of energy levels of ground and excited torsional states were used to produce model spectra obtained with the non-local thermodynamic equilibrium (non-LTE) 3D line radiative transfer code lime. We found that the modelled non-LTE intensities of the CH_3OH lines can be lower by factor of >10-100 than those calculated under assumption of LTE. Though population inversion occurs in the model calculations for many (sub)millimetre transitions, it does not lead to the strong maser amplification and noticeably high line intensities. We identify the strongest CH_3OH (sub)millimetre lines that could be searched for with the Atacama Large Millimeter Array (ALMA) in nearby discs. The two best candidates are the CH_3OH 5_0 - 4_0A^+ (241.791 GHz) and 5_-1 - 4_-1E (241.767 GHz) lines, which could possibly be detected with the ∼5σ signal-to-noise ratio after ∼3 h of integration with the full ALMA array.