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Title:
Carbon Abundance in Small Magellanic Cloud Planetary Nebulae Through Advanced Camera for Surveys Prism Spectroscopy: Constraining Stellar Evolution at Low Metallicity
Authors:
Stanghellini, Letizia; Lee, Ting-Hui; Shaw, Richard A.; Balick, Bruce; Villaver, Eva
Affiliation:
AA(National Optical Astronomy Observatory, 950 N. Cherry Av., Tucson, AZ 85719, USA ), AB(Department of Physics and Astronomy, Western Kentucky University, 1906 College Heights Blvd #11077, Bowling Green, KY 42101, USA ), AC(National Optical Astronomy Observatory, 950 N. Cherry Av., Tucson, AZ 85719, USA ), AD(Astronomy Department, Box 351580, University of Washington, Seattle WA 98195, USA ), AE(Universidad Autónoma de Madrid, Departamento de Física Teórica C-XI, 28049 Madrid, Spain )
Publication:
The Astrophysical Journal, Volume 702, Issue 1, pp. 733-744 (2009). (ApJ Homepage)
Publication Date:
09/2009
Origin:
IOP
ApJ Keywords:
planetary nebulae: general, stars: abundances, stars: evolution, ultraviolet: ISM
DOI:
10.1088/0004-637X/702/1/733
Bibliographic Code:
2009ApJ...702..733S

Abstract

We perform near ultraviolet ACS prism spectroscopy of 11 Small Magellanic Cloud (SMC) planetary nebulae (PNe) with the main aim of deriving the abundance of carbon. The analysis of the ACS spectra provides reliable atomic carbon abundances for all but a couple of our targets; ionic C2+ abundances are calculated for all target PNe. With the present paper we more than double the number of SMC PNe with known carbon abundances, providing a good database to study the elemental evolution in low- and intermediate-mass stars at low metallicity. We study carbon abundances of Magellanic Cloud PNe in the framework of stellar evolution models and the elemental yields. Constraining SMC and LMC stellar evolutionary models is now possible with the present data, through the comparison of the final yields calculated and the CNO abundances observed. We found that SMC PNe are almost exclusively carbon rich, and that for the most part they have not undergone the hot bottom burning phase, contrary to about half of the studied LMC PNe. The yields from stellar evolutionary models with LMC and SMC metallicities broadly agree with the observations. In particular, evolutionary yields for M to < 3.5 M sun well encompass the abundances of round and elliptical PNe in the SMC. We found that the carbon emission lines are major coolants for SMC PNe, more so than in their LMC counterparts, indicating that metallicity has an effect on the physics of PNe, as predicted by Stanghellini et al..
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