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          Institute: MPI für Astronomie     Collection: Publikationen_mpia     Display Documents

ID: 693891.0, MPI für Astronomie / Publikationen_mpia
CANDELS: the progenitors of compact quiescent galaxies at z ~ 2
Authors:Barro, G.; Faber, S. M.; Pérez-González, P. G.; Koo, D. C.; Williams, C. C.; Kocevski, D. D.; Trump, J. R.; Mozena, M.; McGrath, E.; van der Wel, A.; Wuyts, S.; Bell, E. F.; Croton, D. J.; Ceverino, D.; Dekel, A.; Ashby, M. L. N.; Cheung, E.; Ferguson, H. C.; Fontana, A.; Fang, J.; Giavalisco, M.; Grogin, N. A.; Guo, Y.; Hathi, N. P.; Hopkins, P. F.; Huang, K.-H.; Koekemoer, A. M.; Kartaltepe, J. S.; Lee, K.-S.; Newman, J. A.; Porter, L. A.; Primack, J. R.; Ryan, R. E.; Rosario, D.; Somerville, R. S.; Salvato, M.; Hsu, L.-T.
Date of Publication (YYYY-MM-DD):2013
Title of Journal:The Astrophysical Journal
Issue / Number:2
Start Page:id. 104 (11 pp)
Audience:Not Specified
Abstract / Description: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.
Free Keywords:galaxies: high-redshift; galaxies: photometry; galaxies: starburst
External Publication Status:published
Document Type:Article
Communicated by:N. N.
Affiliations:MPI für Astronomie
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