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Wisnioski, E.; Mendel, J. T.; Schreiber, N. M. Förster; Genzel, R.; Wilman, D.; Wuyts, S.; Belli, S.; Beifiori, A.; Bender, R.; Brammer, G.; Chan, J.; Davies, R. I.; Davies, R. L.; Fabricius, M.; Fossati, M.; Galametz, A.; Lang, P.; Lutz, D.; Nelson, E. J.; Momcheva, I.; Rosario, D.; Saglia, R.; Tacconi, L. J.; Tadaki, K.; Uebler, H.; Dokkum, P. G. van (2018): The KMOS3D Survey: Rotating Compact Star-forming Galaxies and the Decomposition of Integrated Line Widths. In: Astrophysical Journal, Vol. 855, No. 2, 97
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Using integral field spectroscopy, we investigate the kinematic properties of 35 massive centrally dense and compact star-forming galaxies (SFGs;log (M) over bar (*)[M-circle dot] = 11.1, log(Sigma(1kpc)[M-circle dot kpc(-2)]) > 9.5 (M-*/r(e)(1.5)[M-circle dot kpc(-1.5)]) > 10.3) at z similar to 0.7-3.7 within the KMOS3D survey. We spatially resolve 23 compact SFGs and find that the majority are dominated by rotational motions with velocities ranging from 95 to 500 km s(-1). The range of rotation velocities is reflected in a similar range of integrated Ha line widths, 75-400 km s(-1), consistent with the kinematic properties of mass-matched extended galaxies from the full KMOS3D sample. The fraction of compact SFGs that are classified as "rotation-dominated" or "disklike" also mirrors the fractions of the full KMOS3D sample. We show that integrated line-of-sight gas velocity dispersions from KMOS3D are best approximated by a linear combination of their rotation and turbulent velocities with a lesser but still significant contribution from galactic-scale winds. The H alpha exponential disk sizes of compact SFGs are, on average, 2.5 +/- 0.2 kpc, 1-2x the continuum sizes, in agreement with previous work. The compact SFGs have a 1.4x higher active galactic nucleus (AGN) incidence than the full KMOS3D sample at fixed stellar mass with an average AGN fraction of 76%. Given their high and centrally concentrated stellar masses, as well as stellar-to-dynamical mass ratios close to unity, the compact SFGs are likely to have low molecular gas fractions and to quench on a short timescale unless replenished with inflowing gas. The rotation in these compact systems suggests that their direct descendants are rotating passive galaxies.