The primordial helium abundance from a new sample of metal-deficient blue compact galaxies

We use high-quality spectrophotometric observations of 10 low- metallicity blue compact galaxies (BCGs) with oxygen abundance ranging from 12 + log (O/H) = 7. 37 to 8. 04 to determine the primordial helium abundance. We take special care into investigating the physical effects which may affect such a determination. We find that underlying stellar absorption, enhancement of helium lines due to self-absorption, and corrections for neutral and doubly ionized helium to be negligible. The main physical mechanism changing the He I line intensities from their recombination values is collisional excitation. To correct for it, we calculate the electron number density in the He^+^ zone by a self- consistent procedure which constrains the He I λ5876/λ4471, λ6678/ λ4471 and λ7065/λ4471 line ratios to have their recombination values, after correction for collisional enhancement. The density sensitive He I λ7065 line plays an important role in this respect. The usual practice of using the electron number density derived from the S II λ6717/λ6731 ratio underestimates the collisional enhancement correction and hence overestimates the helium abundance by ~5%. We find that Brocklehurst's (1972) He I recombination emissivities give a smaller dispersion of the data points in the Y versus O/H and Y versus N/H planes and within the derived He abundances from different lines in a given galaxy than Smits's old (1991a, b) emissivities. The dispersion is comparable when Smits's new (1994) emissivities are used. By taking the mean of the intercepts of both Y versus O/H and Y versus N/H linear regressions at 0/H = N/H = 0, we determine a primordial helium mass fraction Yₚ_ = 0. 229 +/- 0. 004, with Brocklehurst's emissivities, and Yₚ_ = 0. 240 +/- 0. 005 with Smits's new emissivities. Taking the mean Y of the four most metal-deficient BCGs (Z < Zₛun_/15) in our sample gives Yₚ_ = 0. 233 +/- 0. 003 with Brocklehurst's emissivities. Adding the four known BCGs with Z < Zₛun_/15 from the literature yields: Yₚ_ = 0. 232 +/- 0. 002. These determinations are consistent with the lower limit of Yₚ_ = 0. 236 required by standard big bang nucleosynthesis theory. We obtain a slope dY/dZ = 5. 8 +/- 1. 7 with Brocklehurst's emissivities and dY/dZ = 5. 8 +/- 4. 4 with Smits' new emissivities, larger than the values predicted by closed-box models, but consistent with those given by chemical evolution models with differential galactic winds.