A little less than 13.8 billion years ago, our Universe was an infinitesimal point. However, just under four hundred thousand years later, it had become a hot, dense, highly ionized plasma with a temperature of about 5,000 degrees Fahrenheit and a density about 109 times today's value (1). Then something fascinating happened. The plasma underwent a rapid process of recombination, with protons attaching to electrons to form hydrogen, emitting photons with each reaction and providing the fingerprints of today's Universe (2). One of the most interesting aspects of studying these early moments concerns the non-uniformity of the Universe. This non-uniformity, or anisotropy as it is called, is reflected in the inhomogeneous structure of the current Universe. During moments of recombination, energy density fluctuations due to various proposed causes triggered photon scattering. As the Universe expanded, this same inhomogeneity was amplified, meaning that by studying the original diffusion in the photosphere during moments of recombination, the current structure of the Universe can be understood to a large extent (2). In other words, the modern Universe and the microwave background are only “images of the surface of [the] last diffusion” which occurred approximately 378,000 years after the Big Bang (1). So, in this article I will analyze the nature of elementary particles and photons in the Universe at the time of recombination and discuss the possibilities of using a type of scattering known as Compton scattering to help describe the non-uniform structure of the current Universe. The Universe at the time of recombination was theoretically approximated to...... middle of paper ...... modification would have affected the dynamics of the recombination Universe, causing visible distortions 13.8 billion d years later in the form of a non-uniform cosmos. Studying these dynamics closely can give us a much better idea of ​​why the Universe is structured the way it is today and allow us to better hypothesize about what we should look for when studying deep space and galactic structures. However, the effects exhibited by CMB distortions are small and NASA's COBE data were not sensitive enough to detect them. Given the constraints of the new PIXIE mission, the possibility of reconciling these synthesized theories with experimental data seems likely (6). As shown in Figure 3, PIXIE's limitations are much less. If not PIXIE, the Planck mission could also serve this purpose. However, until the data arrives, astrophysics can only wait.