Raymond C. Simons, Susan A. Kassin, Jonathan R. Trump, Benjamin J. Weiner, Timothy M. Heckman, Guillermo Barro, David C. Koo, Yicheng Guo, Camilla Pacifici, Anton Koekemoer, Andrew W. Stephens

Research output: Contribution to journalArticlepeer-review

37 Scopus citations


We present results from a survey of the internal kinematics of 49 star-forming galaxies at z∼2 in the CANDELS fields with the Keck/MOSFIRE spectrograph, Survey in the near-Infrared of Galaxies with Multiple position Angles (SIGMA). Kinematics (rotation velocity Vrot and gas velocity dispersion sg) are measured from nebular emission lines which trace the hot ionized gas surrounding star-forming regions. We find that by z∼2, massive star-forming galaxies (log M∗ Mo ≳ 10.2) have assembled primitive disks: their kinematics are dominated by rotation, they are consistent with a marginally stable disk model, and they form a Tully-Fisher relation. These massive galaxies have values of Vrot δg that are factors of 2-5 lower than local well-ordered galaxies at similar masses. Such results are consistent with findings by other studies. We find that low-mass galaxies (log M∗ Mo ≳10.2) at this epoch are still in the early stages of disk assembly: their kinematics are often dominated by gas velocity dispersion and they fall from the Tully-Fisher relation to significantly low values of Vrot. This kinematic downsizing implies that the process(es) responsible for disrupting disks at z∼2 have a stronger effect and/or are more active in low-mass systems. In conclusion, we find that the period of rapid stellar mass growth at z∼2 is coincident with the nascent assembly of low-mass disks and the assembly and settling of high-mass disks.

Original languageEnglish (US)
Article number14
JournalAstrophysical Journal
Issue number1
StatePublished - Oct 10 2016


  • galaxies: evolution
  • galaxies: formation
  • galaxies: fundamental parameters
  • galaxies: kinematics and dynamics

ASJC Scopus subject areas

  • Astronomy and Astrophysics
  • Space and Planetary Science


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