  The [O II] lambda3727 emission lines and absorption features from stellar
Balmer and Ca H&K lines are the most accessible kinematic diagnotics in
galaxies at z~1. We investigate the kinematics of 22 local late-type galaxies
using these spectral features and we compare the results to 21-cm neutral
hydrogen spectra in order to assess the utility of each diagnostic for
measuring galaxy masses. In order to simulate data at high redshift where only
1-dimensional velocity profiles are normally available, we study spatially
integrated as well as spatially-resolved spectra. Although the studied galaxies
span a wide range of morphological types, inclinations, and star formation
rates, we find that the gaseous and stellar kinematic tracers yield comparable
kinematic line widths and systemic velocities. The [O II] and H I line widths
correlate most strongly, showing an intrinsic dispersion of ~20 km/s, or ~10%
for a typical galaxy with a kinematic width of 200 km/s. In a few extreme
cases, the [O II] line widths underestimate the neutral hydrogen width by 50%.
Reliable velocity widths can also be obtained from the stellar Balmer and Ca
H&K absorption lines, even for some of the very late-type galaxies which have
strong emission lines. The intrinsic dispersion is <10% between the stellar
absorption and H I line widths. We provide a prescription for using these
strong stellar absorption and [O II] emission features to measure the
kinematics, and thus masses, of galaxies in the distant universe.
