The paper uses recent data from the James Webb Space Telescope (JWST) and the NANOGrav Pulsar Timing Array (PTA) to study the evolution of supermassive black hole binaries (SMBHBs). The JWST data show a high fraction of dual active galactic nuclei (AGN) at high redshifts, suggesting that the two black holes in a binary system are active simultaneously, rather than independently. This supports the idea that gas-rich mergers are responsible for concurrent AGN activity. The NANOGrav PTA results indicate that the stochastic gravitational wave strain amplitude is below expectations from dual AGN fractions, suggesting either that binaries stall at separations probed by NANOGrav or that they undergo rapid gas-driven inspirals. The study investigates two aspects of SMBH evolution: the 'final parsec' problem, where binaries stall due to a lack of gas or stars, and the possibility of gas-rich mergers that lead to rapid coalescence. The results suggest that the dual AGN fraction is higher than predicted by simulations, indicating that AGN activity is likely triggered by mergers. The data also support the idea that AGN shine together, implying that mergers drive AGN activity. The paper uses analytical techniques and the BH-halo mass relation to model the expected number of BH mergers and their impact on the gravitational wave background. The results show that the dual AGN fraction is higher than expected, which could be due to either a 'final parsec' stall or gas-rich mergers. The findings suggest that the observed dual AGN fraction is consistent with AGN activity being triggered by mergers, and that the gravitational wave strain is reduced due to rapid inspirals or gas-rich mergers. The study highlights the importance of combining JWST and NANOGrav data to better understand SMBH evolution and feedback mechanisms.The paper uses recent data from the James Webb Space Telescope (JWST) and the NANOGrav Pulsar Timing Array (PTA) to study the evolution of supermassive black hole binaries (SMBHBs). The JWST data show a high fraction of dual active galactic nuclei (AGN) at high redshifts, suggesting that the two black holes in a binary system are active simultaneously, rather than independently. This supports the idea that gas-rich mergers are responsible for concurrent AGN activity. The NANOGrav PTA results indicate that the stochastic gravitational wave strain amplitude is below expectations from dual AGN fractions, suggesting either that binaries stall at separations probed by NANOGrav or that they undergo rapid gas-driven inspirals. The study investigates two aspects of SMBH evolution: the 'final parsec' problem, where binaries stall due to a lack of gas or stars, and the possibility of gas-rich mergers that lead to rapid coalescence. The results suggest that the dual AGN fraction is higher than predicted by simulations, indicating that AGN activity is likely triggered by mergers. The data also support the idea that AGN shine together, implying that mergers drive AGN activity. The paper uses analytical techniques and the BH-halo mass relation to model the expected number of BH mergers and their impact on the gravitational wave background. The results show that the dual AGN fraction is higher than expected, which could be due to either a 'final parsec' stall or gas-rich mergers. The findings suggest that the observed dual AGN fraction is consistent with AGN activity being triggered by mergers, and that the gravitational wave strain is reduced due to rapid inspirals or gas-rich mergers. The study highlights the importance of combining JWST and NANOGrav data to better understand SMBH evolution and feedback mechanisms.