Abstract
Based on the best observations of extragalactic H II regions of low metallicity available in the literature we redetermine the primordial helium abundance, Y[p], taking into account all the observed He I line intensities with the exception of those strongly affected by underlying absorption. We derive He/H, N[e](He II), T[e](He II), and τ (3889) self-consistently. We present results for NGC 346, I Zw 18, and NGC 2363. From these objects we find that Y[p] = 0.2351+/-0.0022.
