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We present measurements of the morphology of star-forming gas in galaxiesfrom the EAGLE simulations, and its alignment relative to stars and dark matter(DM). Imaging of such gas in the radio continuum enables weak lensingexperiments that complement traditional optical approaches. Star-forming gas istypically more flattened than its associated stars and DM, particularly forpresent-day subhaloes of total mass $\sim$$10^{ 12-12.5} \mathrm{M_{ \odot}}$,which preferentially host star-forming galaxies with rotationally-supportedstellar discs. Such systems have oblate, spheroidal star-forming gasdistributions, but in both less- and more-massive subhaloes the distributionstend to be prolate, and its morphology correlates positively and significantlywith that of its host galaxy's stars, both in terms of sphericity andtriaxiality. The minor axis of star-forming gas most commonly aligns with theminor axis of its host subhalo's DM, but often aligns more closely with one ofthe other two principal axes of the DM distribution in prolate subhaloes.Star-forming gas aligns with DM less strongly than is the case for stars, butits morphological minor axis aligns closely with its kinematic axis, affordinga route to observational identification of the unsheared morphological axis.The projected ellipticities of star-forming gas in EAGLE are consistent withshapes inferred from high-fidelity radio continuum images, and they exhibitgreater shape noise than is the case for images of the stars, owing to thegreater characteristic flattening of star-forming gas with respect to stars.

The morphology of star-forming gas and its alignment with galaxies and dark matter haloes in the EAGLE simulations