Orbital spectroscopy allows for the analysis of surface composition on the planet Mars, and is providing evidence for the presence of liquid water throughout the planet’s history. We use hyperspectral images from the Compact Reconnaissance Imaging Spectrometer for Mars (CRISM) aboard the Mars Reconnaissance Orbiter (MRO) to identify a variety of compositions on the planet. These compositions can provide information about the conditions present at the time of their formation. In many cases, as where carbonates are identified, these compositions are clear evidence for the presence of liquid water in the martian past. We identify minerals by their unique absorptions at specific wavelengths through the examination of CRISM surface reflectance data across 438 wavelengths from 1.0 to 3.9 microns. For identification, the CRISM spectra are matched to spectra of laboratory samples from Earth. However, there are differences between these spectra that give some new insight into the combination of minerals present and their formation process. By applying factor analysis to the CRISM dataset where the spectral signature of the mineral components vary independently from one another, the measurements can be expressed as a linear sum of the components. We have applied this target transformation and factor analysis technique to CRISM spectra to identify and isolate the various mineral components present, even under circumstances where the mineral components are only present in minor abundances and mixed with other spectral signatures. Because the entire dataset is used to retrieve mineral spectral signatures, this analysis greatly reduces instrumental error to provide well-defined CRISM spectra. Ultimately, by applying our data analysis technique to the global CRISM dataset, we will have a stronger and more detailed understanding of surface composition and aqueous processes on Mars. Based on these processes we can then invoke different conditions conducive for the development of life on Mars.