  Using the HST/WFC3 and ACS multi-band imaging data taken in CANDELS and
3D-HST, we study the general properties and the diversity of the progenitors of
the Milky Way (MWs) and local massive galaxy (MGs) at 0.5 < z < 3.0, based on a
constant cumulative number density analysis. After careful data reduction and
stacking analysis, we conduct a radially resolved pixel SED fitting to obtain
the radial distributions of the stellar mass and rest-frame colors. The stellar
mass of MWs increases in self-similar way, irrespective of the radial distance,
while that of MGs grows in inside-out way where they obtain ~ 75% of the total
mass at outer (> 2.5 kpc) radius since z ~ 2. Although the radial mass profiles
evolve in distinct ways, the formation and quenching of the central dense
region (or bulge) ahead of the outer disk formation are found to be common for
both systems. The sudden reddening of bulge at z ~ 1.6 and z ~ 2.4 for MWs and
MGs, respectively, suggests the formation of bulge and would give a clue to the
different gas accretion histories and quenching. A new approach to evaluate the
morphological diversity is conducted by using the average surface density
profile and its dispersion. The variety of the radial mass profiles for MGs
peaks at higher redshift (z > 2.8), and then rapidly converges to more uniform
shape at z < 1.5, while that for MWs remains in the outer region over the
redshift. Compared with the observed star formation rates and color profiles,
the evolution of variety is consistently explained by the star formation
activities.
