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We present a detailed analysis of the structure and resolved stellarpopulations of simulated merger remnants, and compare them to observations ofcompact quiescent galaxies at z ~ 2. We find that major merging is a viablemechanism to produce systems of ~ 10^11 Msun and ~ 1 kpc size, provided the gasfraction at the time of final coalescence is high (~ 40%), and provided thatthe progenitors are compact star-forming galaxies, as expected at highredshift. Their integrated spectral energy distributions and velocitydispersions are in good agreement with the observations, and their position inthe (v_{maj}/sigma, ellipticity) diagram traces the upper envelope of thedistribution of lower redshift early-type galaxies. The simulated mergerremnants show time- and sightline-dependent M/L ratio gradients that resultfrom a superposition of radially dependent stellar age, stellar metallicity,and extinction. The median ratio of effective radius in rest-frame V-band lightto that in mass surface density is ~ 2 during the quiescent remnant phase. Thisis typically expressed by a negative color gradient (i.e., red core), which weexpect to correlate with the integrated color of the system. Finally, thesimulations differ from the observations in their surface brightness profileshape. The simulated remnants are typically best fit by high (n >> 4) Sersicindices, whereas observed quiescent galaxies at z ~ 2 tend to be less cuspy(median n ~ 2.3). Limiting early star formation in the progenitors may berequired to prevent the simulated merger remnants from having extended wings.

On Sizes, Kinematics, M/L Gradients, and Light Profiles of Massive Compact Galaxies at z~2