This study investigates deviations from the Planck-ACDM model in the late universe ($z \lesssim 2.5$) using Gaussian Processes (GPs) with minimal assumptions. The authors analyze Cosmic Chronometers (CC), Type Ia Supernovae (SN), and Baryon Acoustic Oscillations (BAO) data to understand where new physics is most relevant. They identify intriguing features at low ($z \lesssim 0.5$) and high ($z \gtrsim 2$) redshifts, with significant deviations between $0.5 \lesssim z \lesssim 2$. The combined CC+SN+BAO dataset reveals insights into dark energy (DE) dynamics, suggesting characteristics beyond quintessence and phantom models. DE exhibits n-quintessence traits at $z \gtrsim 2$, transitioning to phantom traits at $1 \lesssim z \lesssim 2$. The characteristics differ between $H_0$-SH0ES and $H_0$-AkCMB scenarios, with the former leaning towards phantom traits and the latter towards quintessence. The authors suggest exploring new physics at $z \lesssim 0.5$ and $1.5 \lesssim z \lesssim 2.5$, particularly around $z = 2$, to address cosmological tensions such as $H_0$ and $S_8$.This study investigates deviations from the Planck-ACDM model in the late universe ($z \lesssim 2.5$) using Gaussian Processes (GPs) with minimal assumptions. The authors analyze Cosmic Chronometers (CC), Type Ia Supernovae (SN), and Baryon Acoustic Oscillations (BAO) data to understand where new physics is most relevant. They identify intriguing features at low ($z \lesssim 0.5$) and high ($z \gtrsim 2$) redshifts, with significant deviations between $0.5 \lesssim z \lesssim 2$. The combined CC+SN+BAO dataset reveals insights into dark energy (DE) dynamics, suggesting characteristics beyond quintessence and phantom models. DE exhibits n-quintessence traits at $z \gtrsim 2$, transitioning to phantom traits at $1 \lesssim z \lesssim 2$. The characteristics differ between $H_0$-SH0ES and $H_0$-AkCMB scenarios, with the former leaning towards phantom traits and the latter towards quintessence. The authors suggest exploring new physics at $z \lesssim 0.5$ and $1.5 \lesssim z \lesssim 2.5$, particularly around $z = 2$, to address cosmological tensions such as $H_0$ and $S_8$.