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PHL 932: When Is a Planetary Nebula Not a Planetary Nebula?

Published online by Cambridge University Press:  02 January 2013

David J. Frew ,
Greg J. Madsen ,
Simon J. O'Toole  and
Quentin A. Parker
David J. Frew*
Affiliation:
Department of Physics, Macquarie University, NSW 2109 Perth Observatory, Bickley, WA 6076
Greg J. Madsen
Affiliation:
Sydney Institute for Astronomy, School of Physics, University of Sydney, NSW 2006
Simon J. O'Toole
Affiliation:
Anglo–Australian Observatory, PO Box 296, Epping, NSW 1710
Quentin A. Parker
Affiliation:
Department of Physics, Macquarie University, NSW 2109 Anglo–Australian Observatory, PO Box 296, Epping, NSW 1710
*
ECorresponding author. Email: dfrew@physics.mq.edu.au
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Abstract

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The emission nebula around the subdwarf B (sdB) star PHL 932 is currently classified as a planetary nebula (PN) in the literature. Based on a large body of multi-wavelength data, both new and previously published, we show here that this low-excitation nebula is in fact a small Strömgren sphere (Hii region) in the interstellar medium around this star. We summarise the properties of the nebula and its ionizing star, and discuss its evolutionary status. We find no compelling evidence for close binarity, arguing that PHL 932 is an ordinary sdB star. We also find that the emission nebulae around the hot DO stars PG 0108 + 101 and PG 0109 + 111 are also Strömgren spheres in the ISM, and along with PHL 932, are probably associated with the same extensive region of high-latitude molecular gas in Pisces–Pegasus.

Keywords

Hii regionsISM: cloudsplanetary nebulae: generalstars: horizontal-branchstars: individual (PHL 932)subdwarfs
Type
Research Article
Information
Publications of the Astronomical Society of Australia , Volume 27 , Issue 2 , 2010 , pp. 203 - 209
Copyright
Copyright © Astronomical Society of Australia 2010

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