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We use a simple, self-consistent, self-gravitating semi-analytic disc modelto conduct an examination of the parameter space in which self-gravitatingdiscs may exist. We then use Monte-Carlo radiative transfer to generatesynthetic ALMA images of these self-gravitating discs to determine the subsetof this parameter space in which they generate non-axisymmetric structure thatis potentially detectable by ALMA. Recently, several transition discs have beenobserved to have non-axisymmetric structure that extends out to large radii. Ithas been suggested that one possible origin of these asymmetries could bespiral density waves induced by disc self-gravity. We use our simple model tosee if these discs exist in the region of parameter space where self-gravitycould feasibly explain these spiral features. We find that for self-gravity toplay a role in these systems typically requires a disc mass around an order ofmagnitude higher than the observed disc masses for the systems. The spiralamplitudes produced by self-gravity in the local approximation are relativelyweak when compared to amplitudes produced by tidal interactions, or spiralslaunched at Lindblad resonances due to embedded planets in the disc. As such,we ultimately caution against diagnosing spiral features as being due toself-gravity, unless the disc exists in the very narrow region of parameterspace where the spiral wave amplitudes are large enough to produce detectablefeatures, but not so large as to cause the disc to fragment.

Directly observing continuum emission from self-gravitating spiral waves