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The Sulfur Abundance Anomaly in Planetary Nebulae

Published online by Cambridge University Press:  15 December 2006

R. B. C. Henry ,
J. N. Skinner ,
K. B. Kwitter  and
J. B. Milingo
R. B. C. Henry
Affiliation:
H.L. Dodge Department of Physics & Astronomy, University of Oklahoma, Norman, OK 73019 USA email: henry@nhn.ou.edu, skinner@nhn.ou.edu
J. N. Skinner
Affiliation:
H.L. Dodge Department of Physics & Astronomy, University of Oklahoma, Norman, OK 73019 USA email: henry@nhn.ou.edu, skinner@nhn.ou.edu
K. B. Kwitter
Affiliation:
Department of Astronomy, Williams College, Williamstown, MA 01267 USA, email: kkwitter@williams.edu
J. B. Milingo
Affiliation:
Department of Physics & Astronomy, Franklin & Marshall College, Lancaster, PA 17604 USA email: jmilingo@fandm.edu
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The alpha elements O, Ne, Mg, Si, S, Cl, and Ar are produced together in massive stars and their abundances are expected to evolve in lockstep. Both H II regions and planetary nebulae serve as interstellar probes of alpha element abundances. We have measured abundances for the alpha elements O, Ne, S, Cl, and Ar in over 130 Galactic Types I and II and halo PNe in a consistent manner from our own optical (3600–9600Å) spectra (Henry, Kwitter, & Balick 2004). Figure 1 is a plot of Ne vs. O for a combined dataset containing H II regions, blue compact galaxies, and our sample of planetary nebulae. All object types appear to be consistent with the expected linear relation between Ne and O. Similar plots of Cl and Ar vs. O show the same behavior. However, S vs. O is an exception.

Keywords

ISM: planetary nebulae: generalGalaxy: abundances
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 2 , Symposium S234: Planetary Nebulae in our Galaxy and Beyond , April 2006 , pp. 417 - 418
Copyright
© 2006 International Astronomical Union