Dissecting the size evolution of elliptical galaxies since z~1: puffing   up vs minor merging scenarios
  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. 
Ignacio Trujillo, Ignacio Ferreras, Ignacio G. de la Rosa
astro-ph.CO astro-ph.GA