Primordial Helium Abundance: A Reanalysis of the Izotov-Thuan Spectroscopic Sample

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dc.creatorFukugita, Masataka
dc.creatorKawasaki, Masahiro
dc.date2006-03-14
dc.date2006-11-09
dc.date.accessioned2026-07-07T10:43:41Z
dc.date.available2026-07-07T10:43:41Z
dc.descriptionA reanalysis is made for the helium abundance determination for the Izotov-Thuan (2004) spectroscopic sample of extragalactic H II regions. We find that the effect of underlying stellar absorption of the He I lines, which is more important for metal poor systems, affects significantly the inferred primordial helium abundance $Y_p$ obtained in the zero metallicity limit and the slope of linear extrapolation, $dY/dZ$. This brings $Y_p$ from $0.234\pm0.004$ to $0.250\pm 0.004$ and $dY/dZ=4.7\pm 1.0$ to $1.1\pm 1.4$. Conservatively, this indicates the importance of the proper understanding of underlying stellar absorption for accurate determinations of the primordial helium abundance to the error of $δY_p\simeq 0.002-0.004$.
dc.description12 pages, 3 figures, misplaced figures are corrected, typos in Table1 are corrected
dc.identifierhttps://arxiv.org/abs/astro-ph/0603334
dc.identifierhttp://arxiv.org/abs/astro-ph/0603334
dc.identifierAstrophys.J.646:691-695,2006
dc.identifierdoi:10.1086/505109
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/182332
dc.subjectAstrophysics
dc.titlePrimordial Helium Abundance: A Reanalysis of the Izotov-Thuan Spectroscopic Sample
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