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tokens: and magnetic fields, and has been shown to produce realistic galaxy populations in large-scale cosmological boxes (Vogelsberger etal. 2013 ; Genel etal. 2014 ). The most novel aspects of the simulations, with respect to previous studies, are the large simulation sample, high resolution, the inclusion of magnetic fields that are seeded, grown and evolved in a fully cosmological context, and the BH model that has been used in only one simulation set previous to this study (Marinacci etal. 2014a ). The suite comprises 30 simulations with typical baryonic mass resolution of around 510 4 M , three of which have higher resolution counterparts with eight times better mass resolution. The sample size, resolution and galaxy formation model make these simulations some of the most advanced and comprehensive found in the literature. We analysed the properties of the stellar components of these simulations, and found that they lie on the expected stellar masshalo mass relation, and are consistent with other key observables such as flat rotation curves, the massmetallicity relation and present-day SFRs. The simulated galaxies are, on average, slightly too massive in the stellar component, particularly at earlier times such as z 3. This may indicate the need for early stellar feedback (see e.g. Aumer etal. 2013 ; Stinson etal. 2013a ). Such feedback may bring down the stellar masses of our simulations and reduce the number of compact galaxies (see Fig. 5 ), which we will investigate in future work. The mass distributions of our simulated galaxies are realistic and produce rotationally supported discs: most of our simulations have flat rotation curves, with velocities that match the TullyFisher relation for Milky Way-mass galaxies. We note that in the past, it has proven to be difficult to reproduce flat circular velocity curves for galaxy discs in haloes in the virial mass range 1210 12 M (see for example, Stinson etal. 2010 ; Mollitor, Nezri Teyssier 2015 ; Wang etal. 2015 ), although a variety of recent models have achieved some success (Aumer etal. 2013 ; Stinson etal. 2013a ; Marinacci etal. 2014a ; Schaller etal. 2015a ; Colin etal. 2016 ). The circularity distributions indicate that at least two-thirds of the simulations have well-defined, rotationally supported disc components, with disc-total mass ratios of up to 0.60.7 for the most disc-dominated simulations. These are among the highest disc-total mass ratios in the literature, along with Aumer etal. ( 2013 ). The vertical structure of our simulated discs appears to be somewhat thicker than expected from observations in the Milky Way, which may be related to energy from stellar feedback that acts to puff up the gas disc (see Marinacci etal. 2016 ). Rokar etal. ( 2014 ) reported a similar conclusion, although their feedback recipe included radiation feedback that destroyed the morphology of their disc in addition to thickening it. However, the inner discs of our simulations show some consistency