Reanalyzing the He abundance determination in extragalactic HII Regions

Details Reanalyzing the He abundance determination in extragalactic HII Regions Reanalyzing the He abundance determination in extragalactic HII Regions

Nov 2000

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000ign..confe..25g&link_type=abstract

Ionized Gaseous Nebulae. Mexico City November 21- 24, 2000, meeting abstract

Physics

Scientific paper

The importance of a good determination of the primordial He abundance (YP ) has been extensively discussed in the literature. The method generally used to obtain YP was proposed by Peimbert & Torres-Peimbert (1974) and makes use of a correlation between the He mass fraction (Y) and metallicity, extrapolated to zero metallicity. Low-metallicity HII regions are usually analyzed, in order to minimize the contribution from He produced in stars. Since the statistical uncertainties in the determination of YP are very small (~1%), it is essential to discuss possible systematic errors. We will discuss here many possible effects that can lead to systematic errors in the He abundance determination. The line diagnostics proposed in the literature to remove objects with an important ionization correction factor will also be discussed in relation with the starburst age, gas inhomogeneities, and the cloud optical depth.

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