The determination of accurate and precise stellar parameters and chemical abundances of M dwarfs is of prime importance to the study of Galactic chemical evolution, since these are the most abundant stars in the Galaxy. Moreover, M dwarfs are excellent targets, due to their low mass, for searching for small planets. In order to characterize the mass, radius, and bulk composition of a planet, we once more need to have access to precise parameters and to the chemical composition of its host star. The aim of this project is to better characterize this population of poorly known stars via high-resolution near-infrared (NIR) spectroscopy and hence address the two wider research goals set out above.