Hα spectroscopy of galaxies at z > 2:: Kinematics and star formation

We present near-infrared spectroscopy of Halpha emission lines in a sample of 16 star-forming galaxies at redshifts 2.0 < z < 2.6. Our targets are drawn from a large sample of galaxies photometrically selected and spectroscopically confirmed to lie in this redshift range. We have obtained this large sample with an extension of the broadband U(n)GR color criteria used to identify Lyman break galaxies at z similar to 3. The primary selection criterion for IR spectroscopic observation was proximity to a QSO sight line; we therefore expect the galaxies presented here to be representative of the sample as a whole. Six of the galaxies exhibit spatially extended, tilted Halpha emission lines; rotation curves for these objects reach mean velocities of similar to150 km s(-1) at radii of similar to6 kpc, without corrections for inclination or any other observational effect. The velocities and radii give a mean dynamical mass of (M) greater than or equal to 4 x 10(10) M(circle dot). We have obtained archival Hubble Space Telescope images for two of these galaxies; they are morphologically irregular. One-dimensional velocity dispersions for the 16 galaxies range from similar to50 to similar to260 km s(-1), and in cases in which we have both virial masses implied by the velocity dispersions and dynamical masses derived from the spatially extended emission lines, they are in rough agreement. We compare our kinematic results with similar measurements made at z similar to 3 and find that both the observed rotational velocities and velocity dispersions tend to be larger at z similar to 2 than at z similar to 3. We also calculate star formation rates (SFRs) from the Halpha luminosities and compare them with SFRs calculated from the UV continuum luminosity. We find a mean SFR(Halpha) of 16 M(circle dot) yr(-1) and an average SFR(Halpha)/SFR(UV) ratio of 2.4, without correcting for extinction. We see moderate evidence for an inverse correlation between the UV continuum luminosity and the ratio SFR(Halpha)/SFR(UV), such as might be observed if the UV-faint galaxies suffered greater extinction. We discuss the effects of dust and star formation history on the SFRs and conclude that extinction is the most likely explanation for the discrepancy between the two SFRs.