The supernova remnant (SNR) 1604, otherwise known as Kepler’s Supernova, is in the Ophiuchus constellation in the Milky Way Galaxy. It was observed in October 1604, notable for its significant brightness being seen even in daylight for up to three weeks. Previous studies showed ejecta knots traveling upwards of 10,000 km s-1, indicating the remnant is in free expansion. This is unusual for an SNR this old, as current evolution theories predict free expansion ending ~200 years post explosion as the ejecta interacts more with circumstellar material (CSM). Based on archival Chandra data, results are presented from resolved spectral analysis of two regions in the remnant showing high velocities, as well as two regions showing lower velocities. Based on a factor of solar abundance, the elemental abundances observed in Kepler’s spectra were resolved. The electron density and elemental mass was calculated based on the abundances found. Results indicate that electron density and mass do not play a significant role in determining spatial velocities of the ejecta dominated regions. Key Terms: Supernova remnants, X-ray astronomy, Spatial velocity, Mass and density relation
