At spectroscopic resolutions of less than an Angstrom, high resolution techniques can reasonably be attempted to extract chemical compositions from data gathered with the Magellan Echellete (MagE) spectrograph. Since the magnitude limit of MagE can reach significantly fainter stars than can MIKE or the PFS in less time, the instrument can be used to preview chemical compositions of objects that will take significantly longer to observe employing the higher resolution spectrographs. In addition, larger numbers of spectra can be gathered, permitting a spectroscopic "quick-look" at stellar populations. In this talk, I will compare results obtained with MagE and MIKE for some of George's BMP and other stars, and discuss some of the limitations regarding the stellar parameters and chemical compositions that can be derived from the MagE data.