Huertas-Company, M., Bernardi, M., Pérez-González, P. G., Ashby, M. L. N., Barro, G., Conselice, C., Daddi, E., Dekel, A., Dimauro, P., Faber, S. M., Grogin, N. A., Kartaltepe, J. S., Kocevski, D. D., Koekemoer, A. M., Koo, D. C., Mei, S., and Shankar, F. 2016. "Mass assembly and morphological transformations since z ˜ 3 from CANDELS." Monthly Notices of the Royal Astronomical Society, 462 4495–4516. https://doi.org/10.1093/mnras/stw1866.
We quantify the evolution of the stellar mass functions (SMFs) 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 disc-dominated, intermediate two-component bulge disc systems and irregular disturbed galaxies. At z ˜ 2, 80 per cent 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 109 M?. A majority of the star-forming irregulars present at z ˜ 2 undergo a gradual transformation from disturbed to normal spiral disc 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, because the fraction of bulge-dominated star-forming galaxies with M*/M? > 1010.7 reaches 40 per cent at z 2, the SMF of quiescent galaxies above M* is dominated by compact spheroids. Quenching at this early epoch destroys the disc and produces a compact remnant unless the star-forming progenitors at even higher redshifts are significantly more dense. At 1 2, the SMF of quiescent galaxies above M* is dominated by compact spheroids. Quenching at this early epoch destroys the disc and produces a compact remnant unless the star-forming progenitors at even higher redshifts are significantly more dense. At 1 2, the SMF of quiescent galaxies above M* is dominated by compact spheroids. Quenching at this early epoch destroys the disc and produces a compact remnant unless the star-forming progenitors at even higher redshifts are significantly more dense. At 1 2, the SMF of quiescent galaxies above M* is dominated by compact spheroids. Quenching at this early epoch destroys the disc and produces a compact remnant unless the star-forming progenitors at even higher redshifts are significantly more dense. At 1 10 M?. These low-mass galaxies are compact, bulge-dominated systems, which were environmentally quenched: destruction of the disc through ram-pressure stripping is the likely process.
