This paper investigates the presence of dark radiation (DR) in the early Universe using Baryon Acoustic Oscillations (BAO) data from the DESI collaboration. The study focuses on the effective number of neutrinos, $ N_{eff} $, and how it relates to the parameter $ \Delta N_{eff} \equiv N_{eff} - 3.044 $. The research analyzes one-parameter extensions of the $ \Lambda $ CDM model, where DR is either free-streaming or behaves as a perfect fluid due to self-interactions. The results show a significant relaxation of upper bounds on $ \Delta N_{eff} $, with $ \Delta N_{eff} \leq 0.39 $ (95% C.L.) for free-streaming DR and a mild preference for fluid DR, $ \Delta N_{eff} = 0.221_{-0.18}^{+0.088} $ ( $ \leq 0.46 $, 95% C.L.). The study also explores the tension between the $ H_0 $ value inferred from cosmological datasets and the larger value measured from supernovae. The new BAO data from DESI allow for larger abundances of DR, which could help reconcile the $ H_0 $ tension. The results show that the tension with the $ SH_{0}ES $ measurement is less than $ 3\sigma $ for free-streaming DR and as low as $ 2\sigma $ for fluid DR. Combining the DESI data with $ SH_{0}ES $ data provides strong evidence for dark radiation with $ \Delta N_{eff} \simeq 0.6 $ and significant improvements in $ \chi^2 $ over the $ \Lambda $ CDM model. The paper also discusses the impact of primordial element abundances on the constraints on $ \Delta N_{eff} $, and how the production of DR after Big Bang Nucleosynthesis (BBN) can avoid these constraints. The results show that the $ H_0 $ tension is significantly reduced in models where DR is produced after BBN. The study concludes that the new BAO data from DESI provide a robust framework for understanding dark radiation and its implications for the $ H_0 $ tension. The findings suggest that the $ H_0 $ tension can be interpreted as a mild to moderate statistical fluctuation within the $ \Lambda $ CDM + $ \Delta N_{eff} $ models.This paper investigates the presence of dark radiation (DR) in the early Universe using Baryon Acoustic Oscillations (BAO) data from the DESI collaboration. The study focuses on the effective number of neutrinos, $ N_{eff} $, and how it relates to the parameter $ \Delta N_{eff} \equiv N_{eff} - 3.044 $. The research analyzes one-parameter extensions of the $ \Lambda $ CDM model, where DR is either free-streaming or behaves as a perfect fluid due to self-interactions. The results show a significant relaxation of upper bounds on $ \Delta N_{eff} $, with $ \Delta N_{eff} \leq 0.39 $ (95% C.L.) for free-streaming DR and a mild preference for fluid DR, $ \Delta N_{eff} = 0.221_{-0.18}^{+0.088} $ ( $ \leq 0.46 $, 95% C.L.). The study also explores the tension between the $ H_0 $ value inferred from cosmological datasets and the larger value measured from supernovae. The new BAO data from DESI allow for larger abundances of DR, which could help reconcile the $ H_0 $ tension. The results show that the tension with the $ SH_{0}ES $ measurement is less than $ 3\sigma $ for free-streaming DR and as low as $ 2\sigma $ for fluid DR. Combining the DESI data with $ SH_{0}ES $ data provides strong evidence for dark radiation with $ \Delta N_{eff} \simeq 0.6 $ and significant improvements in $ \chi^2 $ over the $ \Lambda $ CDM model. The paper also discusses the impact of primordial element abundances on the constraints on $ \Delta N_{eff} $, and how the production of DR after Big Bang Nucleosynthesis (BBN) can avoid these constraints. The results show that the $ H_0 $ tension is significantly reduced in models where DR is produced after BBN. The study concludes that the new BAO data from DESI provide a robust framework for understanding dark radiation and its implications for the $ H_0 $ tension. The findings suggest that the $ H_0 $ tension can be interpreted as a mild to moderate statistical fluctuation within the $ \Lambda $ CDM + $ \Delta N_{eff} $ models.