Testing cosmological models with the brightness profile of distant
  galaxies
  This work uses observed galaxy surface brightness profiles at high redshifts
to determine the cosmological model best suited to interpret these
observations. Theoretical predictions of galactic surface brightness profiles
are compared to observational data in two cosmological models, $\Lambda$CDM and
Einstein-de Sitter, to calculate the evolutionary effects of different
spacetime geometries in these profiles in order to try to find out if the
available data is capable of indicating the cosmology that best represents
actual galactic brightness profiles observations. Starting from the connection
between the angular diameter distance and the galactic surface brightness as
advanced by Ellis and Perry (1979), we derived scaling relations using data
from the Virgo galactic cluster in order to obtain theoretical predictions of
the galactic surface brightness modeled by the Sersic profile at redshift
values equal to a sample of galaxies in the range $1.5 \lesssim z \lesssim 2.3$
composed by a subset of Szomoru's et al. (2012) observations. We then
calculated the difference between theory and observation in order to determine
the changes required in the effective radius and effective surface brightness
so that the observed galaxies may evolve to have features similar to the Virgo
cluster ones. Our results show that within the data uncertainties of this
particular subset of galaxies it is not possible to distinguish which of the
two cosmological models used here predicts theoretical curves in better
agreement with the observed ones, that is, one cannot identify a clear and
detectable difference in galactic evolution incurred by the galaxies of our
sample when applying each cosmology. We also concluded that the Sersic index
$n$ does not seem to play a significant effect in the evolution of these
galaxies.
