This work focuses on measuring the energy transfer of supermassive black holes (SMBHs) such as Sagittarius A* located at the center of the Milky Way and M87* at the center of the Messier 87 galaxy through the Eddington luminosity, Eddington limit, accretion rate and total mass-energy. To calculate luminosity versus accretion rate with determined efficiency we use photometric data from NASA/IPAC Extragalactic Database and from CDS Portal Database overlaying observational data, and with this, we could infer critical properties such as radiative efficiency and the influence of jet contributions. Luminosity versus accretion rate graph with an Eddington-limited cap visually depicts linear growth of luminosity below the limit and a mass-dependent plateau which reveal drastically different ceilings on their possible steady-state radiative output of these SMBHs. Observed and modeled luminosities for a given accretion rate are much lower than predicted, which suggests that the system is in a radiatively inefficient mode which could imply that a significant fraction of the energy is being channeled into jets or outflows rather than being radiated away. With this, the accretion physics and black hole evolution of how SMBHs grow over cosmic time was resolved through the accretion efficiency and the duty cycle of active versus quiescent phases; as well as contribute with the feedback processes of the energy output from accretion that not only makes the black hole visible across the electromagnetic spectrum but also influences the surrounding environment in the Universe (e.g., heating interstellar gas, driving jets). Accurately modeling this relationship helps in understanding how SMBHs regulate their host galaxies.