The paper investigates the possibility of evolving dark energy using baryon acoustic oscillation (BAO) measurements from the Dark Energy Spectroscopic Instrument (DESI) and other cosmological probes. The authors fit three simple scalar field models—quadratic, linear, and dark energy radiation—to the DESI BAO data, combined with cosmic microwave background (CMB) anisotropy measurements and supernova datasets. They find that a preference for evolving dark energy over a cosmological constant is evident, with the simplest canonical scalar field models fitting the data well. The models exhibit a preference for non-zero kinetic scalar field energy, comprising 2-4% of the total energy density at the 95% confidence level. This preference helps alleviate the mild tension between BAO and supernova measurements under the $\Lambda$CDM model, reducing the tension to $n_{\sigma} < 2.8$. The results suggest that simple canonical scalar fields can successfully explain the DESI BAO measurements without requiring a phantom crossing in the dark energy equation of state.The paper investigates the possibility of evolving dark energy using baryon acoustic oscillation (BAO) measurements from the Dark Energy Spectroscopic Instrument (DESI) and other cosmological probes. The authors fit three simple scalar field models—quadratic, linear, and dark energy radiation—to the DESI BAO data, combined with cosmic microwave background (CMB) anisotropy measurements and supernova datasets. They find that a preference for evolving dark energy over a cosmological constant is evident, with the simplest canonical scalar field models fitting the data well. The models exhibit a preference for non-zero kinetic scalar field energy, comprising 2-4% of the total energy density at the 95% confidence level. This preference helps alleviate the mild tension between BAO and supernova measurements under the $\Lambda$CDM model, reducing the tension to $n_{\sigma} < 2.8$. The results suggest that simple canonical scalar fields can successfully explain the DESI BAO measurements without requiring a phantom crossing in the dark energy equation of state.