Cosmological Constraints from Galaxy Clustering and the Mass-to-Number
  Ratio of Galaxy Clusters: Marginalizing over the Physics of Galaxy Formation
  Many approaches to obtaining cosmological constraints rely on the connection
between galaxies and dark matter. However, the distribution of galaxies is
dependent on their formation and evolution as well as the cosmological model,
and galaxy formation is still not a well-constrained process. Thus, methods
that probe cosmology using galaxies as a tracer for dark matter must be able to
accurately estimate the cosmological parameters without knowing the details of
galaxy formation a priori. We apply this reasoning to the method of obtaining
$\Omega_m$ and $\sigma_8$ from galaxy clustering combined with the
mass-to-number ratio of galaxy clusters. To test the sensitivity of this method
to variations due to galaxy formation, we consider several different models
applied to the same cosmological dark matter simulation. The cosmological
parameters are then estimated using the observables in each model,
marginalizing over the parameters of the Halo Occupation Distribution (HOD). We
find that for models where the galaxies can be well represented by a
parameterized HOD, this method can successfully extract the desired
cosmological parameters for a wide range of galaxy formation prescriptions.
