2009MNRAS.396.1675F

By means of galaxy evolutionary models, we explore the direct consequences of the Λ cold dark matter (ΛCDM) cosmogony on the size evolution of galactic discs, avoiding intentionally the introduction of intermediate (uncertain) astrophysical processes. Based on the shape of the rotation curves and guided by a simplicity criterion, we adopt an average galaxy mass baryon fraction f_gal= 0.03. In order to study general behaviours, only models with the average initial conditions are analysed. The stellar and B-band effective radii, R_* and R_B, of individual galaxies grow significantly with time (inside-out disc formation) with laws that are weakly dependent on stellar mass, M_* or luminosity, L_B. However, the change of R_* with z at a fixed M_* is slow; for z ≤ 2.5, R_*(M_*= constant) ∝ (1 + z)^–0.4 for a large range of masses. On the other hand, the change of R_B with z at a fixed L_B is strong and it resembles the R_B decreasing law of the individual models; roughly R_B(L_B = const) ∝ (1 + z)^–0.85 for z ≲ 0.75, and ∝ (1 + z)^–1.1 for higher zs. We find also that at z = 0, R_*∝ M^0.38_* and R_B ∝ L^0.40_B, remaining the slopes of these relations practically the same up to z ~ 3. Our model predictions are in reasonable agreement with observational inferences on the typical radius change with z of late-type galaxies more luminous (massive) than high values imposed by the selection effects. The models also seem to be consistent, within the large scatter, with the R_B and L_B values obtained from small (non-complete) samples of sub-L_*late-type galaxies with available rest-frame photometric information at different zs. The properties and evolution of the ΛCDM haloes seem to be the main drivers of galaxy disk size evolution. Nevertheless, the models reveal a potential difficulty in explaining the observed steepening of the R_B-L_B relation with respect to the R_*-M_*one, an effect related to the well-established colour-magnitude relation.