Martian meteorites are the only rock samples from Mars that are currently accessible for research in Earth-based laboratories. The meteorites are derived from the near-surface units adjacent to their source craters. These source craters eject material beyond the martian escape velocity during formation from random, hypervelocity impact on the planet’s surface. Specific source craters for any of the martian meteorites are unknown. This study uses results from a queried database to constrain potential source craters based on parameters such as ejection age, petrology, preservation, and crater diameter. Preliminary results indicate a number of candidate source craters that require detailed mapping to better understand their morphology, relative age, and volcanic context.
