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Estimating the binary fraction of planetary nebulae central stars

Published online by Cambridge University Press:  30 August 2012

D. Douchin ,
O. De Marco ,
D. J. Frew ,
G. H. Jacoby ,
J.-C. Passy ,
T. Hillwig ,
S. B. Howell ,
H. Bond ,
A. Peyaud  and
A. Zijlstra
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D. Douchin
Affiliation:
Macquarie University Research Centre in Astronomy, Astrophysics & Astrophotonics Department of Physics & Astronomy, Macquarie University Australia GRAAL, UniversitéMontpellier 2, France
O. De Marco
Affiliation:
Macquarie University Research Centre in Astronomy, Astrophysics & Astrophotonics Department of Physics & Astronomy, Macquarie University Australia
D. J. Frew
Affiliation:
Macquarie University Research Centre in Astronomy, Astrophysics & Astrophotonics Department of Physics & Astronomy, Macquarie University Australia
G. H. Jacoby
Affiliation:
Giant Magellan Telescope, USA
J.-C. Passy
Affiliation:
University of Victoria, Canada American Museum of Natural History, New York City, USA
T. Hillwig
Affiliation:
Valparaiso University, USA
S. B. Howell
Affiliation:
NASA Ames Research Center, USA
H. Bond
Affiliation:
Space Telescope Science Institute, USA
A. Peyaud
Affiliation:
Macquarie University Research Centre in Astronomy, Astrophysics & Astrophotonics
A. Zijlstra
Affiliation:
University of Manchester, UK
R. Napiwotzki
Affiliation:
University of Hertfordshire, UK
G. Jasniewicz
Affiliation:
GRAAL, UniversitéMontpellier 2, France
Q. Parker
Affiliation:
Macquarie University Research Centre in Astronomy, Astrophysics & Astrophotonics Department of Physics & Astronomy, Macquarie University Australia
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Abstract

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During the past 20 years, the idea that non-spherical planetary nebulae might need a binary or planetary interaction to be shaped was discussed by various authors. It is now generally agreed that the varied morphologies of planetary nebulae cannot be fully explained solely by single star evolution. Observationally, more binary central stars of planetary nebulae have been discovered, opening new possibilities to understand the connections between binarity and morphology. So far, ≃45 binary central stars of planetary nebulae have been detected, most being close systems detected via flux variability. In order to determine the PN binary fraction, one needs a method that can detect wider binaries. We present here recent results concentrating on binary infrared excess observations aimed at detecting binaries of any separation.

Keywords

techniques: radial velocitiestechniques: photometricbinaries: generalstars: statisticsplanetary nebulae: general
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 7 , Symposium S283: Planetary Nebulae: An Eye to the Future , July 2011 , pp. 346 - 347
Copyright
Copyright © International Astronomical Union 2012

References

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Jacoby, G. H. et al. 2010, PASA, 27, 156 CrossRefGoogle Scholar
Miszalski, B. et al. 2009, A&A, 505, 249 Google Scholar