  We infer the local stellar-to-halo/subhalo mass relations (MRs) for central
and satellite galaxies separately. We constraint this relations by using
several combinations of observational data, consisting of the total galaxy
stellar mass function, its decomposition into centrals and satellites, and the
projected two-point correlation functions measured in different stellar mass
bins. The differences among the resulting MRs are within the model-fit
uncertainties (which are very small, smaller than the intrinsic scatter between
galaxy and halo mass), no matter what combination of data are used. We also
constrain the values of the intrinsic scatter around the central-halo (CH) and
satellite-subhalo (SS) MRs assuming them to be constant: sigma_c= 0.168+-0.051
dex and sigma_s = 0.172+-0.057 dex, respectively. The CH and SS MRs are
actually different, in particular when we take the subhalo mass at the
present-day epoch instead of at their accretion time. We calculate several
population statistics. We find that the central galaxy is not on average within
the mass distribution of the most-massive satellite, even for cluster-sized
halos, i.e., centrals are not a mere realization of the high-end of the
satellite mass function; however for > 3x10^13 msun halos, ~15% of centrals
could be. We also find that the probabilities of MW-sized halos of having N
Magellanic-Clouds (MCs)-sized satellites agree well with observational
measures; for a halo mass of 2x10^12 msun, the probability to have 2 MCs is
5.4%, but if we exclude those systems with satellites larger than the MCs, then
the probability decreases to <2.2%.
