general population including low-metallicity subdwarfs, low surface gravity objects, and potentially cloudy/cloudless L dwarfs (@Burgasser03 [@Burgasser04; @Burgasser07]; @Looper08; @Cruz09; @Cushing09; @Kirkpatrick10; @Rice10; @Radigan12).

The most relevant sub-population to giant exoplanet studies are young (i.e., low surface gravity) isolated L dwarfs. The archetypal low surface gravity L dwarf, 2MASSJ01415823$-$4633574 (2M0141), was discovered by @Kirkpatrick06. Its optical spectrum exhibits strong bands of VO but abnormally weak TiO, K, and Na absorption. In the near-infrared, its red $J-K_{s}$ color (2MASS $J-K_{s}$=1.73) and triangular $H$-band spectral morphology distinguish it from field L dwarfs (@Kirkpatrick10; @Patience12). It is suspected to be a member of the $\beta$ Pictoris or Tucana-Horologium association, although the precise kinematics required to confirm association have not yet been determined (@Kirkpatrick10). After the discovery and characterization of 2M0141, additional isolated L dwarfs sharing similar photometric and spectral peculiarities attributed to a low surface gravity were reported (e.g. @Reid08; @Cruz09; @Kirkpatrick10). While the ages of these seemingly young L dwarfs remain largely unconstrained, there are kinematic and spatial indications that they represent the lowest mass members of nearby moving groups such as AB Doradus, $\beta$ Pictoris, Tucana-Horalogium (@Cruz09; @Kirkpatrick10).

@Cruz09 point out that the majority of objects defining the population of the lowest 