  We have analysed the distribution of galaxies in groups identified in the
largest redshift surveys at the present: the final release of the 2dF Galaxy
Redshift Survey and the first release of the Sloan Digital Sky Survey. Our work
comprises the study of the galaxy density profiles and the fraction of galaxies
per spectral type as a function of the group-centric distance. We have
calculated the projected galaxy density profiles of galaxy groups using
composite samples in order to increase the statistical significance of the
results. Special cares have been taken in order to avoid possible biases in the
group identification and the construction of the projected galaxy density
profile estimator. The results show that the projected galaxy density profiles
obtained for both redshift surveys are in agreement with a projected Navarro,
Frenk & White predictions in the range $0.15< r/r_{200}
  < 1$, whereas a good fit for the measured profiles in the whole range of
$r/r_{200}$ is given by a projected King profile. We have adopted a generalized
King profile to fit the measured projected density profiles per spectral type.
In order to infer the 3-D galaxy density profiles, we deproject the 2-D density
profiles using a deprojection method similar to the developed by Allen &
Fabian. From 2-D and 3-D galaxy density profiles we have estimated the
corresponding galaxy fractions per spectral type. The 2-D fraction of galaxies
computed using the projected profiles show a similar segregation of galaxy
spectral types as the obtained by Dom\'{\i}nguez et al. for groups in the early
data release of the 2dF Galaxy Redshift Survey. As expected, the trends
obtained for the 3-D galaxy fractions show steeper slopes than the observed in
the 2-D fractions.
