The4He Abundance in the Metal‐deficient Blue Compact Dwarf Galaxies Tol 1214−277 and Tol 65

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Abstract
We present high-quality Keck telescope spectroscopic observations of the two metal-deficient blue compact dwarf (BCD) galaxies Tol 1214-277 and Tol 65. These data are used to derive the heavy-element and helium abundances. We find that the oxygen abundances in Tol 1214-277 and Tol 65 are the same, 12 + log = 7.54 ± 0.01, or Z☉/24, despite the different ionization conditions in these galaxies. The nitrogen-to-oxygen abundance ratio in both galaxies is log = -1.64 ± 0.02 and lies in the narrow range found for the other most metal-deficient BCDs. We use the five strongest He I emission lines λλ3889, 4471, 5876, 6678, and 7065 to self-consistently correct their intensities for collisional and fluorescent enhancement mechanisms and to derive the 4He abundance. Underlying stellar absorption is found to be important for the He I λ4471 emission line in both galaxies, being larger in Tol 65. The weighted 4He mass fractions in Tol 1214-277 and Tol 65 are, respectively, Y = 0.2458 ± 0.0039 and 0.2410 ± 0.0050 when the three He I emission lines λλ4471, 5876, and 6678 are used and are, respectively, Y = 0.2466 ± 0.0043 and 0.2463 ± 0.0057 when the He I λ4471 emission line is excluded. These values are in very good agreement with recent measurements of the 4He mass fraction in others of the most metal-deficient BCDs by Izotov et al. We find that the combined effect of the systematic uncertainties due to the underlying He I stellar absorption lines, ionization, and temperature structure of the H II region and collisional excitation of the hydrogen emission lines is likely small, not exceeding ~2% (the error is 2 σ). Our results support the validity of the standard big bang model of nucleosynthesis.
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