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Title:
Sulfur, Chlorine, and Argon Abundances in Planetary Nebulae. III. Observations and Results for a Final Sample
Authors:
Kwitter, K. B.; Henry, R. B. C.; Milingo, J. B.
Affiliation:
AA(Department of Astronomy, Williams College, Williamstown, MA 01267; ), AB(Department of Physics and Astronomy, University of Oklahoma, Norman, OK 73019; .; Visiting Astronomer, Cerro Tololo Inter-American Observatory, National Optical Astronomy Observatory, which is operated by the Association of Universities for Research in Astronomy (AURA), Inc., under cooperative agreement with the National Science Foundation.), AC(Department of Physics and Astronomy, University of Oklahoma, Norman, OK 73019; .; Department of Physics, Gettysburg College, Gettysburg, PA 17325; .)
Publication:
The Publications of the Astronomical Society of the Pacific, Volume 115, Issue 803, pp. 80-95. (PASP Homepage)
Publication Date:
01/2003
Origin:
UCP
PASP Keywords:
ISM: Abundances, ISM: Planetary Nebulae: General, Stars: Evolution
DOI:
10.1086/345108
Bibliographic Code:
2003PASP..115...80K

Abstract

This paper is the fourth in a series whose purpose is to study the interstellar abundances of sulfur, chlorine, and argon in the Galaxy using a sample of 86 planetary nebulae. Here we present new high-quality spectrophotometric observations of 20 Galactic planetary nebulae with spectral coverage from 3700 to 9600 Å. A major feature of our observations throughout the entire study has been the inclusion of the near-infrared lines of [S III] λλ9069, 9532, which allows us to calculate accurate S+2 abundances and to either improve upon or convincingly confirm results of earlier sulfur abundance studies. For each of the 20 objects here, we calculate ratios of S/O, Cl/O, and Ar/O and find average values of S/O=(1.1+/-1.1)×10-2, Cl/O=(4.2+/-5.3)×10-4, and Ar/O=(5.7+/-4.3)×10-3. For six objects, we are able to compare abundances of S+3 calculated directly from available [S IV] 10.5 μm measurements with those inferred indirectly from the values of the ionization correction factors for sulfur. In the final paper of the series, we will compile results from all 86 objects, search for and evaluate trends, and use chemical evolution models to interpret our results.
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