Presentation Abstract: The center of our Milky Way Galaxy, better known as the Galactic Center, is host to many important and influential landmarks, including the supermassive black hole Sgr A*, stellar complexes like Sgr B, and many young ultraviolet light producing stars. The stellar radiated output produced by these stars is absorbed by the dust and gas present in the ambient medium around these stars. This radiation produced by stars gives rise to ionized H II regions, which then emit through bremsstrahlung emission (free-free emission). Bremsstrahlung emission occurs when electrons scatter off ions without being captured, so they are free before and after interaction. Another emission component seen in the Galactic Center is synchrotron emission, which is produced by energetic electrons generated from the jet of the supermassive black hole and supernova remnants, spiraling around magnetic field lines. Any object that is hot gives off light, or thermal emission. When the ultraviolet radiation from stars is absorbed by the dust, the dust is heated, and then re-radiates as thermal emission at far-infrared wavelengths. Using the three previous emission components, this environment was analyzed in order to identify three main features in the Galactic Center: ionized gas, magnetic fields and dust. Bremsstrahlung emission was used to trace H II regions (ionized gas), synchrotron emission was used to trace magnetic field lines, and thermal emission was used to trace the dust. After tracing these spectral features, they were displayed, resulting in a map of the Galactic Center showing all three of these features that can be used for further analysis in the near future.