SINFONI Integral Field Spectroscopy ofz∼ 2 UV‐selected Galaxies: Rotation Curves and Dynamical Evolution

We present ~0 5 resolution near-infrared integral field spectroscopy of the Hα line emission of 14 z ~ 2 UV-selected BM/BX galaxies, obtained with SINFONI at the ESO Very Large Telescope. The average Hα half-light radius is r 1/2 ≈ 4 h kpc, and line emission is detected over ≳20 h kpc in several sources. In nine galaxies, we detect spatially resolved velocity gradients, from 40 to 410 km s -1 over ~10 h kpc. The kinematics of the larger systems are generally consistent with orbital motions. Four galaxies are well described by rotating clumpy disks, and we extracted rotation curves out to radii ≳10 h kpc. One or two galaxies exhibit signatures more consistent with mergers. Analyzing all 14 galaxies in the framework of rotating disks, we infer mean inclination- and beam-corrected maximum circular velocities of v c ~ 180 ± 90 km s -1 and dynamical masses from ~0.5 to 25 × 10 10 h M ☉ within r 1/2 . The specific angular momenta of our BM/BX galaxies are similar to those of local late-type galaxies. Moreover, the specific angular momenta of their baryons are comparable to those of their dark matter halos. Extrapolating from the average v c at 10 h kpc, the virial mass of the typical halo of a galaxy in our sample is 10 11.7±0.5 h M ☉ . Kinematic modeling of the three best cases implies a ratio of v c to local velocity dispersion v c /σ ~ 2-4 and, accordingly, a large geometric thickness. We argue that this suggests a mass accretion (alternatively, gas exhaustion) timescale of ~500 Myr. We also argue that if our BM/BX galaxies were initially gas-rich, their clumpy disks would subsequently lose their angular momentum and form compact bulges on a timescale of ~1 Gyr.