Geometry of Star-forming Galaxies from SDSS, 3D-HST, and CANDELS
Ferguson, H. C.; Giavalisco, M.; Brammer, G.; Rix, H. -W.; Faber, S. M.; van der Wel, A.; Franx, M.; van Dokkum, P. G.; Holden, B. P.; Bell, E. F.; Dekel, A.; Koo, D. C.; Skelton, R.; Momcheva, I.; Mozena, M.; Martig, M.; Whitaker, K.; Primack, J.; Ceverino, D.; Chang, Yu-Yen; Kassin, S. A.
Germany, United States, South Africa, Israel, Spain, Netherlands
Abstract
We determine the intrinsic, three-dimensional shape distribution of star-forming galaxies at 0 < z < 2.5, as inferred from their observed projected axis ratios. In the present-day universe, star-forming galaxies of all masses 109-1011 M ⊙ are predominantly thin, nearly oblate disks, in line with previous studies. We now extend this to higher redshifts, and find that among massive galaxies (M * > 1010 M ⊙) disks are the most common geometric shape at all z <~ 2. Lower-mass galaxies at z > 1 possess a broad range of geometric shapes: the fraction of elongated (prolate) galaxies increases toward higher redshifts and lower masses. Galaxies with stellar mass 109 M ⊙ (1010 M ⊙) are a mix of roughly equal numbers of elongated and disk galaxies at z ~ 1 (z ~ 2). This suggests that galaxies in this mass range do not yet have disks that are sustained over many orbital periods, implying that galaxies with present-day stellar mass comparable to that of the Milky Way typically first formed such sustained stellar disks at redshift z ~ 1.5-2. Combined with constraints on the evolution of the star formation rate density and the distribution of star formation over galaxies with different masses, our findings imply that, averaged over cosmic time, the majority of stars formed in disks.
Based on observations with the Hubble Space Telescope, obtained at the Space Telescope Science Institute, which is operated by AURA, Inc., under NASA contract NAS 5-26555.