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We report on nine wide common proper motion systems containing late-type M,L, or T companions. We confirm six previously reported companions, and identifythree new systems. The ages of these systems are determined using diagnosticsfor both stellar primaries and low--mass secondaries and masses for thesecondaries are inferred using evolutionary models. Of our three newdiscoveries, the M3+T6.5 pair G 204-39 and SDSS J1758+4633 has an ageconstrained to 0.5-1.5 Gyr making the secondary a potentially useful browndwarf benchmark. The G5+L4 pair G 200-28 and SDSS J1416+5006 has a projectedseparation of ~25,000 AU making it one of the widest and lowest binding energysystems known to date. The system containing NLTT 2274 and SDSS J0041+1341 isan older M4+L0 (>4.5 Gyr) pair which shows Halpha activity in the secondary butnot the primary making it a useful tracer of age/mass/activity trends. We finda resolved binary frequency for widely-separated (> 100 AU) low--masscompanions (i.e. at least a triple system) which is at least twice thefrequency found for the field ultracool dwarf population. The ratio of triplesto binaries and quadruples to binaries is also high for this sample: 3:5 and1:4, respectively, compared to 8-parsec sample values of 1:4 and 1:26. Theadditional components in these wide companion systems indicates a formationmechanism that requires a third or fourth component to maintain gravitationalstability or facilitate the exchange of angular momentum. The binding energiesfor the nine multiples discussed in this text are among the lowest known forwide low-mass systems, suggesting that weakly bound, low--to--intermediate mass(0.2M_sun < M_tot <1.0M_sun) multiples can form and survive to exist in thefield (1-8 Gyr).

The Brown Dwarf Kinematics Project (BDKP). II. Details on Nine Wide Common Proper Motion Very Low-Mass Companions to Nearby Stars