The minor role of gas-rich major mergers in the rise of intermediate-mass early types at z <~ 1

Details The minor role of gas-rich major mergers in the rise of intermediate-mass early types at z <~ 1 The minor role of gas-rich major mergers in the rise of intermediate-mass early types at z <~ 1

2009-12-03

arxiv.org/abs/0912.0700v2

ApJ, 710, 1170 (2010)

Astronomy and Astrophysics

Astrophysics

Cosmology and Extragalactic Astrophysics

Matches published version in ApJ. 16 pages, 4 figures, 5 tables

Scientific paper

10.1088/0004-637X/710/2/1170

We study the evolution of galaxy structure since z ~ 1 to the present. From a GOODS-S multi-band catalog we define (blue) luminosity- and mass-weighted samples, limited by M_B <= -20 and M_star >= 10^10 M_Sun, comprising 1122 and 987 galaxies, respectively. We extract early-type (E/S0/Sa) and late-type (Sb-Irr) subsamples by their position in the concentration-asymmetry plane, in which galaxies exhibit a clear bimodality. We find that the early-type fraction, f_ET, rises with cosmic time, with a corresponding decrease in the late-type fraction, f_LT, in both luminosity- and mass-selected samples. However, the evolution of the comoving number density is very different: the decrease in the total number density of M_B <= -20 galaxies since z = 1 is due to the decrease in the late-type population, which accounts for ~75% of the total star-formation rate in the range under study, while the increase in the total number density of M_star >= 10^10 M_Sun galaxies in the same redshift range is due to the evolution of early types. This suggests that we need a structural transformation between late-type galaxies that form stars actively and early-type galaxies in which the stellar mass is located. Comparing the observed evolution with the gas-rich major merger rate in GOODS-S, we infer that only ~20% of the new early-type galaxies with M_star >= 10^10 M_Sun appeared since z ~ 1 can be explained by this kind of mergers, suggesting that minor mergers and secular processes may be the driving mechanisms of the structural evolution of intermediate-mass (M_star ~ 4x10^10 M_Sun) galaxies since z ~ 1.

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