Investigations in the 60'ies about the question how the Chandrasekhar limit is modified by allowing a self-gravitating mass of cold fermions to rotate seem to have come to the conclusion that the limiting mass is only increased by percents or at most a few tens of percents.
I want to confront this conclusion with the multitude of rotating pressureless self-gravitating disk solutions (to Euler or Vlasov-Poisson equation). The mass of these solutions is not bounded above and -wonder oh wonder!- we do not even need any pressure to counteract the gravitation pull. Rotation suffices to do the job. Granted, none of these solutions seem to be dynamically stable, even to linear perturbations. But already since Jacobi opened his mind to his famous ellipsoids we've learned not to constrain ourselves to strictly stationary configurations.
This leads me to ask two questions:
Q1: Where -in the theoretical arena- does rotation fail to significantly increase the Chandrasekhar limit?
Q2: Can I not see a typical spiral galaxy (e.g. our own) as a single pressureless supermassive star, its flagrant violation of Chandrasekhar's bound due to rotation?