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We investigate the disc-halo connection in massive (Mstar/Msun>5e10) discgalaxies from the cosmological hydrodynamical simulations EAGLE andIllustrisTNG, and compare it with that inferred from the study of HI rotationcurves in nearby massive spirals from the Spitzer Photometry and AccurateRotation Curves (SPARC) dataset. We find that discrepancies between the thesimulated and observed discs arise both on global and on local scales.Globally, the simulated discs inhabit halos that are a factor ~4 (in EAGLE) and~2 (in IllustrisTNG) more massive than those derived from the rotation curveanalysis of the observed dataset. We also use synthetic rotation curves of thesimulated discs to demonstrate that the recovery of the halo masses fromrotation curves are not systematically biased. We find that the simulationspredict dark-matter dominated systems with stellar-to-total enclosed massratios that are a factor of 1.5-2 smaller than real galaxies at all radii. Thisis an alternative manifestation of the `failed feedback problem', since itindicates that simulated halos hosting massive discs have been too inefficientat converting their baryons into stars, possibly due to an overly efficientstellar and/or AGN feedback implementation.

Massive disc galaxies in cosmological hydrodynamical simulations are too dark matter-dominated