Alpha Element Abundances in a Large Sample of Galactic Planetary Nebulae

Details Alpha Element Abundances in a Large Sample of Galactic Planetary Nebulae Alpha Element Abundances in a Large Sample of Galactic Planetary Nebulae

2010-02-18

arxiv.org/abs/1002.3606v1

Astrophysical Journal 711 (2010) 619-630

Astronomy and Astrophysics

Astrophysics

Solar and Stellar Astrophysics

12 pages, 18 figures, 7 tables (note: tables 2-5 are available online only in machine-readable form)

Scientific paper

We present emission line strengths, abundances, and element ratios (X/O for Ne, S, Cl, and Ar) for a sample of 38 Galactic disk planetary nebulae (PNe) consisting primarily of Peimbert classification Type I. Spectrophotometry for these PNe incorporates an extended optical/near-IR range of 3600-9600 angstroms including the [S III] lines at 9069 and 9532. We have utilized Emission Line Spectrum Analyzer, a five-level atom abundance routine, to determine T_e, N_e, ionization correction factors, and total element abundances. With a compilation of data from >120 Milky Way PNe, we present results from our most recent analysis of abundance patterns in Galactic disk PNe. We have examined the alpha elements against H II regions and blue compact galaxies (H2BCG) to discern signatures of depletion or enhancement in PNe progenitor stars, particularly the destruction or production of O and Ne. We present evidence that many PNe have higher Ne/O and lower Ar/Ne ratios compared to H2BCGs within the range of 8.5-9.0 for 12 + log(O/H). This suggests that Ne is being synthesized in the low- and intermediate-mass progenitors. Sulfur abundances in PNe continue to show great scatter and are systematically lower than those found in H2BCG at a given metallicity. Although we find that PNe do show some distinction in alpha elements when compared to H2BCG, within the Peimbert classification types studied, PNe do not show significant differences in alpha elements amongst themselves, at least to an extent that would distinguish in situ nucleosynthesis from the observed dispersion in abundance ratios.

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