2005ApJ...632L..61O

We measure radial gradients of the Mg₂index in 15 E-E/S0 and 14 S0 galaxies. Our homogeneous data set covers a large range of internal stellar velocity dispersions (2.0<logσ<2.5) and Mg₂gradients [{utri}Mg₂/{utri}logr/r^*_e up to -0.14 mag/dex]. We find for the first time a noticeable lower boundary in the relation between Mg₂gradient and σ along the full range of σ, which may be populated by galaxies predominantly formed by monolithic collapse. At high σ, galaxies showing flatter gradients could represent objects that suffered either important merging episodes or later gas accretion. These processes contribute to the flattening of the metallicity gradients, and their increasing importance could define the distribution of the objects above the boundary expected by the ``classical'' monolithic process. This result is in marked contrast to previous works, which found a correlation between {utri}Mg₂/{utri}logr/r^*_eand σ confined to the low-mass galaxies, suggesting that only galaxies below some limiting σ were formed by collapse, whereas the massive ones were formed by mergers. We show observational evidence that a hybrid scenario could also arise among massive galaxies. Finally, we estimate {utri}[Z/H] from Mg₂and Hβ measurements and single stellar population models. The conclusions remain the same, indicating that the results cannot be ascribed to age effects on Mg₂.