Do Baryons Alter the Halos of Low Surface Brightness Galaxies?
  High-quality observations of dark matter-dominated low surface brightness
(LSB) galaxies indicate that, in contrast to the triaxial,
centrally-concentrated cuspy halos formed in collisionless simulations of halo
assembly, these galaxies reside in round, roughly constant density cored halos.
In order to reconcile these data with galaxy formation in the context of LCDM,
processes that alter the shape and density structure of the inner halo are
required. We compile observational properties of LSB galaxies to evaluate the
plausibility that a previously higher baryonic mass content and feedback from
star formation can modify the dark matter halos of these galaxies. We also
compare the properties of bulgeless disk galaxies formed in recent simulations
to the LSB galaxy sample. We find that observational constraints on LSB galaxy
star formation histories, structure, and kinematics make it difficult for
baryonic physics to sphericalize and decrease the central density of the dark
matter halos of LSB galaxies.
