CANDELS: The Progenitors of Compact Quiescent Galaxies at z ~ 2
Barro, Guillermo; Pérez-González, Pablo G.; Bell, Eric F.; Ferguson, Henry C.; Fontana, Adriano; Giavalisco, Mauro; Grogin, Norman A.; Hathi, Nimish P.; Kartaltepe, Jeyhan S.; Kocevski, Dale D.; Koekemoer, Anton M.; Somerville, Rachel S.; Trump, Jonathan R.; van der Wel, Arjen; Faber, S. M.; Williams, Christina C.; Wuyts, Stijn; Huang, Kuang-Han; Ryan, Russell E.; Ashby, M. L. N.; Lee, Kyoung-Soo; Dekel, Avishai; Koo, David C.; Hopkins, Philip F.; Newman, Jeffrey A.; Guo, Yicheng; Primack, Joel R.; Salvato, Mara; Hsu, Li-Ting; Cheung, Edmond; Rosario, David; Ceverino, Daniel; Mozena, Mark; McGrath, Elizabeth; Croton, Darren J.; Fang, Jerome; Porter, Lauren A.
United States, Spain, Germany, Australia, Israel, Italy
Abstract
We combine high-resolution Hubble Space Telescope/WFC3 images with multi-wavelength photometry to track the evolution of structure and activity of massive (M sstarf > 1010 M ⊙) galaxies at redshifts z = 1.4-3 in two fields of the Cosmic Assembly Near-infrared Deep Extragalactic Legacy Survey. We detect compact, star-forming galaxies (cSFGs) whose number densities, masses, sizes, and star formation rates (SFRs) qualify them as likely progenitors of compact, quiescent, massive galaxies (cQGs) at z = 1.5-3. At z >~ 2, cSFGs present SFR = 100-200 M ⊙ yr-1, yet their specific star formation rates (sSFR ~ 10-9 yr-1) are typically half that of other massive SFGs at the same epoch, and host X-ray luminous active galactic nuclei (AGNs) 30 times (~30%) more frequently. These properties suggest that cSFGs are formed by gas-rich processes (mergers or disk-instabilities) that induce a compact starburst and feed an AGN, which, in turn, quench the star formation on dynamical timescales (few 108 yr). The cSFGs are continuously being formed at z = 2-3 and fade to cQGs down to z ~ 1.5. After this epoch, cSFGs are rare, thereby truncating the formation of new cQGs. Meanwhile, down to z = 1, existing cQGs continue to enlarge to match local QGs in size, while less-gas-rich mergers and other secular mechanisms shepherd (larger) SFGs as later arrivals to the red sequence. In summary, we propose two evolutionary tracks of QG formation: an early (z >~ 2), formation path of rapidly quenched cSFGs fading into cQGs that later enlarge within the quiescent phase, and a late-arrival (z <~ 2) path in which larger SFGs form extended QGs without passing through a compact state.