Nearby, young moving groups are ideal testbeds for studying stellar and planetary evolution. By definition, stars in a given moving group should not have significantly different ages or compositions, therefore one can see how the cluster evolves as a function of mass. Additionally, planetary systems around these young stars are still contracting, and thus are bright in the H and K photometric bands. For this reason, moving groups have become attractive targets for planet searches since the masses of photometrically discovered planets are well constrained from the ages of the host moving group (see Biller et al. 2013).  Currently, moving groups are largely characterized based on youth indicators (e.g. lithium absorption, X-ray emission) and space velocities. In this talk, I will discuss recent results which more fully characterize moving groups based on (1) Chemical homogeneity, (2) Origin, and (3) Isochronal Age. These traits have been tested on the well established AB Doradus moving group and the newly discovered Octans-Near moving group. I will show that these methods provide a detailed picture of the AB Doradus group, however, Octans-Near remains difficult to characterize. I will also discuss the future of this technique on low mass members using high resolution H and K spectroscopy.