  Mergers of stellar-mass black holes on highly eccentric orbits are among the
targets for ground-based gravitational-wave detectors, including LIGO, VIRGO,
and KAGRA. These sources may commonly form through gravitational-wave emission
in high velocity dispersion systems or through the secular Kozai-Lidov
mechanism in triple systems. Gravitational waves carry information about the
binaries' orbital parameters and source location. Using the Fisher matrix
technique, we determine the measurement accuracy with which the
LIGO-VIRGO-KAGRA network could measure the source parameters of eccentric
binaries using a matched filtering search of the repeated burst and eccentric
inspiral phases of the waveform. We account for general relativistic precession
and the evolution of the orbital eccentricity and frequency during the
inspiral. We find that the signal-to-noise ratio and the parameter measurement
accuracy may be significantly higher for eccentric sources than for circular
sources. This increase is sensitive to the initial pericenter distance, the
initial eccentricity, and component masses. For instance, compared to a 30
Msun-30 Msun non-spinning circular binary, the chirp mass and sky localization
accuracy can improve for an initially highly eccentric binary by a factor of
~129 (38) and ~2 (11) assuming an initial pericenter distance of 20 Mtot (10
Mtot).
