I will review recent progress on the observational determination of the primordial helium
abundance (Yp). Presently, the best constraints on Yp come from observations of star
forming regions in very metal-poor galaxies (although the impact of Yp on the CMB
has been detected). Progress has come through the discovery of more very metal-poor
galaxies and by extending spectral observations in to the near infrared with, for example,
the Large Binocular Telescope.