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The Nature of the Low Metallicity PN: SBS 1150+599A (=G135.9+55.9)

Published online by Cambridge University Press:  15 December 2006

G. H. Jacoby ,
P. M. Garnavich ,
H. E. Bond ,
A. Noriega-Crespo ,
J. Quinn ,
J. S. Gallagher  and
D. Garcia-Galili
G. H. Jacoby
Affiliation:
WIYN Observatory, 950 N. Cherry Ave., Tucson, AZ 85712, USA email: jacoby@wiyn.org
P. M. Garnavich
Affiliation:
Dept. of Physics, 225 Nieuwland Science Hall, Univ of Notre Dame, Notre Dame, IN 46556, email: pgarnavi@nd.edu, jgallag3@nd.edu
H. E. Bond
Affiliation:
STScI, 3700 San Martin Dr., Baltimore, MD 21218, email: bond@stsci.edu
A. Noriega-Crespo
Affiliation:
SIRTF Science Center, Caltech, 220-6, Pasadena, CA 91125, email: alberto@ipac.caltech.edu
J. Quinn
Affiliation:
Dept. of Physics, 225 Nieuwland Science Hall, Univ of Notre Dame, Notre Dame, IN 46556, email: pgarnavi@nd.edu, jgallag3@nd.edu
J. S. Gallagher
Affiliation:
Dept. of Physics, 225 Nieuwland Science Hall, Univ of Notre Dame, Notre Dame, IN 46556, email: pgarnavi@nd.edu, jgallag3@nd.edu
D. Garcia-Galili
Affiliation:
Marlboro College, South Road, Marlboro, VT 05344
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Abstract

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We have observed SBS 1150+599A spectroscopically in the UV using HST to derive C/H $\sim$ 7.6 and N/H $\sim$ 7.0 for the first time. The central star temperature is now better constrained to $\sim$130,000K, but still is not well determined. This uncertainty dominates the error in O/H, which has been the subject of debate, yet with these data, SBS 1150+599A has the lowest O/H of any PN. Furthermore, the physics of this object are so extreme that minor differences in atomic modeling impact the composition analysis strongly. We also find that the binary central star, based on photometric and kinematic variations, exhibits CV-like properties with an amplitude of 13% and an orbital period of 3.924 hours.

Keywords

abundancesCVbinary
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 2 , Symposium S234: Planetary Nebulae in our Galaxy and Beyond , April 2006 , pp. 431 - 432
Copyright
© 2006 International Astronomical Union