The Stellar , Gas And

We present analysis of the near-infrared spectra of 114 rest-frame UV-selected star-forming galaxies at z ∼ 2. By combining the Hα spectra with photometric measurements from observed 0.3–8 μm, we assess the relationships between kinematics, dynamical masses, inferred gas fractions, and stellar masses and ages. The Hα line widths give a mean velocity dispersion σ = 101 ± 5 km s and a mean dynamical mass Mdyn = 6.9± 0.6× 10 10 M⊙ within a typical radius of ∼ 6 kpc, after excluding AGN. The average dynamical mass is ∼ 2 times larger than the average stellar mass, and the two are correlated at the 2.5σ level and agree to within a factor of several for most objects, consistent with observational and systematic uncertainties. However, ∼ 15% of the sample has Mdyn ≫ M⋆. These objects are best fit by young stellar populations and tend to have high Hα equivalent widths WHα & 200 Å, suggesting that they are young starbursts with large gas masses. Rest-frame optical luminosity and velocity dispersion are correlated with 4σ significance; the correlation and its accompanying large scatter suggest that the processes which produce the correlation between luminosity and velocity dispersion in local galaxies are underway at z ∼ 2. Fourteen of the 114 galaxies in the sample have spatially resolved and tilted Hα emission lines indicative of velocity shear. It is not yet clear whether the shear indicates merging or rotation, but if the galaxies are rotating disks and follow relations between velocity dispersion and circular velocity similar to those seen in local galaxies, our observations underestimate the circular velocities by an average factor of ∼ 2 and the sample has 〈Vc〉 ∼ 190 km s −1 . Using the local empirical correlation between star formation rate per unit area and gas surface density, we estimate the mass of the gas associated with star formation, and find a mean gas fraction of ∼ 50% and a strong decrease in gas fraction with increasing stellar mass. The masses of gas and stars combined are considerably better correlated with the dynamical masses than are the stellar masses alone, and agree to within a factor of three for 85% of the sample. The combination of kinematic measurements, estimates of gas masses, and stellar population properties suggest that the factor of ∼ 500 range in stellar mass across the sample cannot be fully explained by intrinsic differences in the total masses of the galaxies, which vary by a factor of ∼ 40; the remaining variation is due to the evolution of the stellar population and the conversion of gas into stars. Subject headings: galaxies: evolution — galaxies: high redshift – galaxies: kinematics and dynamics