  We have explored the buildup of the local mass-size relation of elliptical
galaxies using two visually classified samples. At low redshift we compiled a
subsample of 2,656 elliptical galaxies from SDSS, whereas at higher redshift
(up to z~1) we extracted a sample of 228 object from the HST/ACS images of the
GOODS. All the galaxies in our study have spectroscopic data, allowing us to
determine the age and mass of the stellar component. Using the fossil record
information contained in the stellar populations of our local sample, we do not
find any evidence for an age segregation at a given stellar mass depending on
the size of the galaxies. At a fixed dynamical mass there is only a <9% size
difference in the two extreme age quartiles of our sample. Consequently, the
local evidence does not support a scenario whereby the present-day mass-size
relation has been progressively established via a bottom-up sequence, where
older galaxies occupy the lower part this relation, remaining in place since
their formation. We find a trend in size that is insensitive to the age of the
stellar populations, at least since z~1. This result supports the idea that the
stellar mass-size relation is formed at z~1, with all galaxies populating a
region which roughly corresponds to 1/2 of the present size distribution. The
fact that the evolution in size is independent of stellar age, together with
the absence of an increase in the scatter of the relationship with redshift
does not support the puffing up mechanism. The observational evidence, however,
can not reject at this stage the minor merging hypothesis. We have made an
estimation of the number of minor merger events necessary to bring the high-z
galaxies into the local relation compatible with the observed size evolution.
Since z=0.8, if the merger mass ratio is 1:3 we estimate ~3+-1 minor mergers
and if the ratio is 1:10 we obtain ~8+-2 events.
