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Spitzer finds cosmic neon's and sulfur's sweet spot: part III, NGC 6822

Published online by Cambridge University Press:  09 March 2010

R. H. Rubin ,
I. A. McNabb ,
J. P. Simpson ,
R. J. Dufour ,
A. W. A. Pauldrach ,
S. W. J. Colgan ,
T. W. Craven ,
E. D. Gitterman  and
C. C. Lo
R. H. Rubin
Affiliation:
NASA Ames Research Center, M.S. 245-6, Moffett Field, CA 94035-1000, USA email: rubin@cygnus.arc.nasa.gov Orion Enterprises Kavli Institute for Astronomy & Astrophysics, Peking University
I. A. McNabb
Affiliation:
NASA Ames Research Center, M.S. 245-6, Moffett Field, CA 94035-1000, USA email: rubin@cygnus.arc.nasa.gov Kavli Institute for Astronomy & Astrophysics, Peking University
J. P. Simpson
Affiliation:
NASA Ames Research Center, M.S. 245-6, Moffett Field, CA 94035-1000, USA email: rubin@cygnus.arc.nasa.gov
R. J. Dufour
Affiliation:
Rice University
A. W. A. Pauldrach
Affiliation:
University Munich
S. W. J. Colgan
Affiliation:
NASA Ames Research Center, M.S. 245-6, Moffett Field, CA 94035-1000, USA email: rubin@cygnus.arc.nasa.gov
T. W. Craven
Affiliation:
NASA Ames Research Center, M.S. 245-6, Moffett Field, CA 94035-1000, USA email: rubin@cygnus.arc.nasa.gov
E. D. Gitterman
Affiliation:
NASA Ames Research Center, M.S. 245-6, Moffett Field, CA 94035-1000, USA email: rubin@cygnus.arc.nasa.gov
C. C. Lo
Affiliation:
NASA Ames Research Center, M.S. 245-6, Moffett Field, CA 94035-1000, USA email: rubin@cygnus.arc.nasa.gov
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Abstract

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We observed several H ii regions in the dwarf irregular galaxy NGC 6822 using the infrared spectrograph on the Spitzer Space Telescope. Our aim is twofold: first, to examine the neon to sulfur abundance ratio in order to determine how much it may vary and whether or not, it is fairly ‘universal’; second, to discriminate and test the predicted ionizing spectral energy distribution between various stellar atmosphere models by comparing with our derivation of the ratio of fractional ionizations involving neon and sulfur. This work extends our previous similar studies of H ii regions in M83 and M33 to lower metallicities.

Keywords

ISM: abundancesH ii regionsstars: atmospheresgalaxies: individual (NGC 6822)
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 5 , Symposium S265: Chemical Abundances in the Universe: Connecting First Stars to Planets , August 2009 , pp. 249 - 250
Copyright
Copyright © International Astronomical Union 2010

References

Killen, R. M. & Dufour, R. J. 1982, PASP 94, 444CrossRefGoogle Scholar
Lebouteiller, V., Bernard-Salas, J., Brandl, B. R., Whelan, D. G., Wu, Y., Charmandaris, V., Devost, D., & Houck, J. R. 2008, ApJ 680, 398CrossRefGoogle Scholar
Rubin, R. H., et al. 2007, MNRAS 377, 1407CrossRefGoogle Scholar
Rubin, R. H., et al. 2008, MNRAS 387, 45CrossRefGoogle Scholar
Simpson, J. P., Rubin, R. H., Colgan, S. W. J., Erickson, E. F., & Haas, M. R. 2004, ApJ 611, 338CrossRefGoogle Scholar
Wu, Y., Bernard-Salas, J., Charmandaris, V., Lebouteiller, V., Hao, L., Brandl, B. R., & Houck, J. R. 2008, ApJ 673, 193CrossRefGoogle Scholar