  We present rotational velocities for individual components of eleven very low
mass (VLM) binaries with spectral types between M7 and L7.5. These results are
based on observations taken with the near-infrared spectrograph, NIRSPEC, and
the Keck II laser guide star adaptive optics (LGS AO) system. We find that the
observed sources tend to be rapid rotators (vsini > 10 km/s), consistent with
previous seeing-limited measurements of VLM objects. The two sources with the
largest vsini, LP 349-25B and HD 130948C, are rotating at ~30% of their break
up speed, and are among the most rapidly rotating VLM objects known.
Furthermore, five binary systems, all with orbital semi-major axes <3.5 AU,
have component vsini values that differ by greater than 3sigma. To bring the
binary components with discrepant rotational velocities into agreement would
require the rotational axes to be inclined with respect to each other, and that
at least one component is inclined with respect to the orbital plane.
Alternatively, each component could be rotating at a different rate, even
though they have similar spectral types. Both differing rotational velocities
and inclinations have implications for binary star formation and evolution. We
also investigate possible dynamical evolution in the triple system HD
130948A-BC. The close binary brown dwarfs B and C have significantly different
vsini values. We demonstrate that components B and C could have been torqued
into misalignment by the primary star, A, via orbital precession. Such a
scenario can also be applied to another triple system in our sample, GJ
569A-Bab. Interactions such as these may play an important role in the
dynamical evolution of very low mass binaries. Finally, we note that two of the
binaries with large differences in component vsini, LP 349-25AB and 2MASS
0746+20AB, are also known radio sources.
