2010MNRAS.407..181C

In this paper, we present simulated observations of massive self-gravitating circumstellar discs using the Atacama Large Millimetre/sub-millimetre Array (ALMA). Using a smoothed particle hydrodynamics model of a 0.2-M_☉disc orbiting a 1-M_☉protostar, with a cooling model appropriate for discs at temperatures below ∼ 160K and representative dust opacities, we have constructed maps of the expected emission at sub-mm wavelengths. We have then used the Common Astronomy Software Applications ALMA simulator to generate simulated images and visibilities with various array configurations and observation frequencies, taking into account the expected thermal noise and atmospheric opacities. We find that at 345GHz (870µm) spiral structures at a resolution of a few au should be readily detectable in approximately face-on discs out to distances of the Taurus-Auriga star-forming complex.