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In this paper we present simulated Atacama Large Millimetre/sub-millimetreArray (ALMA) observations of self-gravitating circumstellar discs withdifferent properties in size, mass and inclination, located in four of the mostextensively studied and surveyed star-forming regions. Starting from a SmoothedParticle Hydrodynamics (SPH) simulation and representative dust opacities, wehave initially constructed maps of the expected emission at sub-mm wavelengthsof a large sample of discs with different properties. We have then simulatedrealistic observations of discs as they may appear with ALMA using the CommonAstronomy Software Application ALMA simulator. We find that, with a propercombination of antenna configuration and integration time, the spiral structurecharacteristic of self-gravitating discs is readily detectable by ALMA over awide range of wavelengths at distances comparable to TW Hydrae ($\sim 50\,$pc), Taurus - Auriga and Ophiucus ($\sim 140 \,$pc) star-forming regions.However, for discs located in Orion complex ($\sim 400 \,$pc) only the largestdiscs in our sample (outer radius of 100 au) show a spatially resolvedstructure while the smaller ones (outer radius of 25 au) are characterized by aspiral structure that is not conclusively detectable with ALMA.

How to Detect the Signatures of Self-Gravitating Circumstellar Discs with the Atacama Large Millimetre/sub-millimetre Array