  We have used NSF's Karl G. Jansky Very Large Array (VLA) to observe a sample
of five known radio-emitting late L and T dwarfs ranging in age from ~0.2 -
3.4Gyr. We observed each target for seven hours, extending to higher
frequencies than previously attempted and establishing proportionally higher
limits on maximum surface magnetic field strengths. Detections of circularly
polarized pulses at 8 - 12~GHz yield measurements of 3.2 - 4.1 kG localized
magnetic fields on four of our targets, including the archetypal cloud variable
and likely planetary-mass object T2.5 dwarf SIMP J01365663+0933473. We
additionally detect a pulse at 15 - 16.5 GHz for the T6.5 dwarf 2MASS
10475385+2124234, corresponding to a localized 5.6 kG field strength. For the
same object, we tentatively detect a 16.5 - 18 GHz pulse, corresponding to a
localized 6.2 kG field strength. We measure rotation periods between ~1.47 -
2.28 hr for 2MASS J10430758+2225236, 2MASS J12373919+6526148, and SDSS
J04234858-0414035, supporting (i) an emerging consensus that rapid rotation may
be important for producing strong dipole fields in convective dynamos and/or
(ii) rapid rotation is a key ingredient for driving the current systems
powering auroral radio emission. We observe evidence of variable structure in
the frequency-dependent time series of our targets on timescales shorter than a
rotation period, suggesting a higher degree of variability in the current
systems near the surfaces of brown dwarfs. Finally, we find that age, mass, and
temperature together cannot account for the strong magnetic fields produced by
our targets.
