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Galaxy Sizes Since $z=2$ from the Perspective of Stellar Mass Distribution within Galaxies

How stellar mass assembles within galaxies is still an open question. We present measurements of the stellar mass distribution on kpc-scale for $\sim5500$ galaxies with stellar masses above $\log(M_{\ast}/M_{\odot})\geqslant9.8$ up to the redshift $2.0$. We create stellar mass maps from Hubble Space Telescope observations by means of the pixel-by-pixel SED fitting method. These maps are used to derive radii encompassing $20\%$, $50\%$, and $80\%$ ($r_{20}$, $r_{50}$ and $r_{80}$) of the total stellar mass from the best-fit Sérsic models. The reliability and limitations of the structural parameter measurements are checked extensively using a large sample ($\sim3000$) of simulated galaxies. The size-mass relations and redshift evolution of $r_{20}$, $r_{50}$ and $r_{80}$ are explored for star-forming and quiescent galaxies. At fixed mass, the star-forming galaxies do not show significant changes in their $r_{20}$, $r_{50}$ and $r_{80}$ sizes, indicating self-similar growth. Only above the pivot stellar mass of $\log(M_{\ast}/M_{\odot})\simeq10.5$, $r_{80}$ evolves as $r_{80}\propto(1+z)^{-0.85\pm0.20}$, indicating that mass builds up in the outskirts of these systems (inside-out growth). The Sérsic values also increase for the massive star-forming galaxies towards late cosmic time. Massive quiescent galaxies show stronger size evolution at all radii, in particular the $r_{20}$ sizes. For these massive galaxies, Sérsic values remain almost constant since at least $z\sim1.3$, indicating that the strong size evolution is related to the changes in the outer parts of these galaxies. We make all the structural parameters publicly available.