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Integral field spectroscopy of galaxies at redshift z~2 has revealed apopulation of early-forming, rotationally-supported disks. These high-redshiftsystems provide a potentially important clue to the formation processes thatbuild disk galaxies in the universe. A particularly well-studied example is thez=2.38 galaxy BzK-15504, which was shown by Genzel et al. (2006) to be arotationally supported disk despite the fact that its high star formation rateand short gas consumption timescale require a very rapid acquisition of mass.Previous kinematical analyses have suggested that z~2 disk galaxies likeBzK-15504 did not form through mergers because their line-of-sight velocityfields display low levels of asymmetry. We perform the same kinematicalanalysis on a set of simulated disk galaxies formed in gas-rich mergers of thetype that may be common at high redshift, and show that the remnant disksdisplay low velocity field asymmetry and satisfy the criteria that have beenused to classify high-redshift galaxies as disks observationally. Further, wecompare one of our remnants to the bulk properties of BzK-15504 and show thatit has a star formation rate, gas surface density, and a circularvelocity-to-velocity dispersion ratio that matches BzK-15504 remarkably well.We suggest that observations of high-redshift disk galaxies like BzK-15504 areconsistent with the hypothesis that gas-rich mergers play an important role indisk formation at high redshift.

High-Redshift Galaxy Kinematics: Constraints on Models of Disk Formation