Using the Hubble Space Telescope ( HST ) /WFC3 and Advanced Camera for Surveys multi-band imaging data taken in CANDELS and 3D-HST , we study the general properties and 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 spectral energy distribution 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 an inside-out way where they obtain \sim 75 \% of the total mass at outer ( > 2.5 kpc ) radius since z \sim 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 the bulge at z \sim 1.6 and z \sim 2.4 for MWs and MGs , respectively , suggests the formation of the 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 a 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 .