The precision measurement of the primordial helium abundance Y_p is a powerful probe of the early Universe. The most common way to determine Y_p is the analyses of observations of metal-poor HII regions found in blue compact dwarf galaxies. We present the spectroscopic sample of 100 HII regions collected from the Sloan Digital Sky Survey. The final analysed sample consists of our sample and HeBCD data base from Izotov et al. (2007). We use a self-consistent procedure to determine physical conditions, current helium abundances, and metallicities of the HII regions. From a regression to zero metallicity, we have obtained Y_p = 0.2462 ± 0.0022, which is one of the most stringent constraints obtained with such methods up to date and is in a good agreement with the Planck result Y_p^Planck=0.2471i±0.0003Y_p^Planck=0.2471±0.0003 . Using the determined value of Y_p and the primordial deuterium abundance taken from Particle Data Group (Zyla et al. 2020) we put a constraint on the effective number of neutrino species N_eff = 2.95 ± 0.16, which is consistent with the Planck one N_eff = 2.99 ± 0.17. Further increase of statistics potentially allows us to achieve Planck accuracy, which in turn will become a powerful tool for studying the self-consistency of the standard cosmological model and/or physics beyond.

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Page created on March 24, 2021.