Papers › Mass assembly and morphological transformations since z∼3 from CANDELS
Mass assembly and morphological transformations since z∼3 from CANDELS
M. Huertas-Company, M. Bernardi, P. G. Pérez-González, M. L. N. Ashby, G. Barro, C. Conselice, E. Daddi, A. Dekel, P. Dimauro, S. M. Faber, N. A. Grogin, J. S. Kartaltepe, D. D. Kocevski, A. M. Koekemoer, D. C. Koo, S. Mei, F. Shankar
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[abridged] We quantify the evolution of the stellar mass functions of star-forming and quiescent galaxies as a function of morphology from z∼3 to the present. Our sample consists of ~50,000 galaxies in the CANDELS fields (∼880 arcmin²), which we divide into four main morphological types, i.e. pure bulge dominated systems, pure spiral disk dominated, intermediate 2-component bulge+disk systems and irregular disturbed galaxies. Our main results are: Star-formation: At z∼2, 80\% of the stellar mass density of star-forming galaxies is in irregular systems. However, by z∼0.5, irregular objects only dominate at stellar masses below 10⁹M⊙. A majority of the star-forming irregulars present at z∼2 undergo a gradual transformation from disturbed to normal spiral disk morphologies by z∼1 without significant interruption to their star-formation. Rejuvenation after a quenching event does not seem to be common except perhaps for the most massive objects. Quenching: We confirm that galaxies reaching a stellar mass of M_*∼10^(10.8)M_⊙ (M^*) tend to quench. Also, quenching implies the presence of a bulge: the abundance of massive red disks is negligible at all redshifts over 2~dex in stellar mass. However the dominant quenching mechanism evolves. At z>2, the SMF of quiescent galaxies above M^* is dominated by compact spheroids. Quenching at this early epoch destroys the disk and produces a compact remnant unless the star-forming progenitors at even higher redshifts are significantly more dense. At 1<z<2, the majority of newly quenched galaxies are disks with a significant central bulge. This suggests that mass-quenching at this epoch starts from the inner parts and preserves the disk. At z<1, the high mass end of the passive SMF is globally in place and the evolution mostly happens at stellar masses below 10¹⁰M_⊙.
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