The coevolution between supermassive black holes and dark matter halos has been examined within the past decade for validity. I have reexamined this coevolution through utilizing a unique method that involves a series of correlations. The first correlation is a relationship between the masses of supermassive black holes of galaxies and their respected galaxy buige masses. The second correlation is a relationship between the masses of galaxy bulges and the circular rotation velocities of the galaxies. By utilizing these two correlations, an indirect relationship between supermassive black holes and dark matter halos can be accomplished. In order to represent the dark matter halos in the galaxies, I chose to use the circular rotation velocity of these galaxies because matter on the outskirts of galaxies is influenced by hypothesized dark matter halos that cause it to rotate around the centers of galaxies at higher velocities than the theoretical values suggest. I used Microsoft Excel to gather and store all of the data gathered to create the two correlations. Data for supermassive black hole masses and galaxy bulge masses of galaxies in solar masses were obtained from Kormendy & Ho (2013), and the MASSIVE Galaxy Survey. Data for the

circular rotation velocities (km/sec) of galaxies were obtained from Bovy et al. (2012), Schulze & Gebhardt (2013), Sun et al. (2013), Kormendy & Ho (2013), and Saliba et al. (2015). A direct relationship was obtained between galaxy bulge mass on the x-axis and supermassive black hole mass on the y-axis. The R^2 value for that relationship was 57.00% . This R^2 value is similar to other papers who have made the same correlation and proven it to exist. The next correlation involves the galaxy bulges and circular rotation velocities of galaxies. The same data for the galaxy bulges was used for this correlation with data from Bovy et al. (2012), Schulze & Gebhardt (2013), Sun et al. (2013), Kormendy & Ho (2013), and Saliba et al. (2015) for circular rotation velocity. I plotted circular rotation velocity on the x-axis and galaxy bulge mass on the y-axis. After segregating the data by their morphologies (Ellipticals, Spirals, or Lenticulars), I took the R^2 values of each set of galaxies and concluded that a valid correlation with an R^2 of 61.95% for the lenticulars was prevalent. My results lead to a greater understanding of dark matter and influences on baryonic matter in galaxies. The knowledge gained from my discovery will better prepare humankind for inhabiting other planets in different galaxies. My findings can be further studied to understand how the matter within galaxies forms sun-like stars that have habitable planets. Another future study would be to delve into how dark matter influences the evolution of lenticular galaxies and if the evolution of dark matter in the galactic disk is the reason why the star formation in lenticular galaxies shut off.