Recent photometric and spectroscopic studies indicate that globular clusters generally are composed of multiple populations. Hence, they radically break with the long-lasting paradigm of considering globular clusters as prime examples for so-called simple stellar populations. Seeking answers to questions about the formation mechanisms of such multiple populations in globular clusters raises the need for detailed spectroscopic analyses of the chemical composition of these stellar systems. In this talk I will present our recent chemical abundance study of four giant stars associated with NGC 6426, one of the most metal-poor Galactic globular clusters known. First, I will briefly introduce EWCODE, a tool we developed in order to accurately and reproducibly determine equivalent widths from spectra like our high-resolution MIKE data. After spending some time discussing the methods applied to derive stellar parameters and subsequently chemical abundances, I will show our results for 22 chemical elements. Among others, we found imprints from hypernova nucleosynthesis as well as from a yet unknown lighter element primary process (LEPP). Finally, tentative evidence for the existence of two chemically distinct subpopulations in NGC 6426 will be discussed.