2009MNRAS.400..766C

Early-type galaxies (ETGs) define a narrow strip in the size-mass plane because of the observed correlation between the effective radius R_eff and the total stellar mass M_*. When expressed in logarithmic units, a linear relation, logR_eff∝ γ logM_*, is indeed observationally found, but the slope γ deviates from the canonical γ = 1/2 value which can be naively predicted for a spherically symmetric isotropic system. We propose here that a transfer of angular momentum to the stellar component induces an anisotropy in the velocity space, thus leading to a modified distribution function (DF). Assuming an Osipkov-Merritt like anisotropic DF, we derive an analytic relation between the slope γ of the size-mass relation and the slope α of the angular momentum term in the DF. With this simple model, we are then able to recover the observed γ value provided α is suitably set. It turns out that an anisotropy profile which is tangential inside ∼ 0.6r_a and radial outside, with r_a the anisotropy radius, is able to reproduce the observed size-mass relation observed for massive (M_* ≥ 2x10¹⁰ h^–1 M_☉) elliptical galaxies.