Active Galactic Nuclei (AGN) feedback is a process where energy and radiation from the central black hole interact with the interstellar medium of its host galaxy, influencing star formation and accretion. This feedback can explain the observed correlation between black hole mass and host galaxy mass. Two main modes of AGN feedback are identified: the radiative mode (quasar or wind mode) and the kinetic mode (radio jet or maintenance mode). The radiative mode, which occurs when the AGN is highly luminous, is less well observed but may involve radiation pressure on dust, driving gas out of the galaxy. The kinetic mode, more commonly observed, involves jets that heat the intracluster medium, reducing cooling and star formation. Observational evidence for the kinetic mode is found in the form of bubbles in the hot gas of cool core clusters. These bubbles, powered by jets from the central black hole, can heat the gas and maintain a balance between heating and cooling. Powerful jetted radio outbursts may also affect galaxy cores. New telescopes and instruments will enhance observational data on all AGN feedback modes. The radiative mode is linked to the black hole mass-stellar velocity dispersion relation, as it relies on radiative efficiency near the Eddington limit. Observational evidence for AGN feedback is strongest in massive galaxies like Brightest Cluster Galaxies (BCGs), where kinetic feedback prevents excessive gas accumulation. AGN feedback is crucial in maintaining the balance between heating and cooling in galaxies, and its role in galaxy evolution is supported by simulations. The kinetic mode is well observed in clusters, with bubbles in the intracluster medium. The radiative mode is less understood but may involve dust-driven winds. Observational studies of AGN winds and outflows show that they can eject gas from galaxies, influencing star formation. The balance between heating and cooling is maintained through AGN feedback, with the kinetic mode playing a dominant role in massive galaxies. The long-term behavior of AGN and their feedback mechanisms may mirror those of stellar mass binary black holes, with radiative efficiency at high luminosity and jet-driven activity at low luminosity. Future observations will provide more insights into AGN feedback across different modes.Active Galactic Nuclei (AGN) feedback is a process where energy and radiation from the central black hole interact with the interstellar medium of its host galaxy, influencing star formation and accretion. This feedback can explain the observed correlation between black hole mass and host galaxy mass. Two main modes of AGN feedback are identified: the radiative mode (quasar or wind mode) and the kinetic mode (radio jet or maintenance mode). The radiative mode, which occurs when the AGN is highly luminous, is less well observed but may involve radiation pressure on dust, driving gas out of the galaxy. The kinetic mode, more commonly observed, involves jets that heat the intracluster medium, reducing cooling and star formation. Observational evidence for the kinetic mode is found in the form of bubbles in the hot gas of cool core clusters. These bubbles, powered by jets from the central black hole, can heat the gas and maintain a balance between heating and cooling. Powerful jetted radio outbursts may also affect galaxy cores. New telescopes and instruments will enhance observational data on all AGN feedback modes. The radiative mode is linked to the black hole mass-stellar velocity dispersion relation, as it relies on radiative efficiency near the Eddington limit. Observational evidence for AGN feedback is strongest in massive galaxies like Brightest Cluster Galaxies (BCGs), where kinetic feedback prevents excessive gas accumulation. AGN feedback is crucial in maintaining the balance between heating and cooling in galaxies, and its role in galaxy evolution is supported by simulations. The kinetic mode is well observed in clusters, with bubbles in the intracluster medium. The radiative mode is less understood but may involve dust-driven winds. Observational studies of AGN winds and outflows show that they can eject gas from galaxies, influencing star formation. The balance between heating and cooling is maintained through AGN feedback, with the kinetic mode playing a dominant role in massive galaxies. The long-term behavior of AGN and their feedback mechanisms may mirror those of stellar mass binary black holes, with radiative efficiency at high luminosity and jet-driven activity at low luminosity. Future observations will provide more insights into AGN feedback across different modes.