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The Population of Debris Discs Orbiting Subgiants

Published online by Cambridge University Press:  06 January 2014

Amy Bonsor
Affiliation:
UJF-Grenoble 1 / CNRS-INSU, Institut de Plantologie et d'Astrophysique de Grenoble (IPAG)UMR 5274, Grenoble, F-38041, France email: amy.bonsor@gmail.com
Grant M. Kennedy
Affiliation:
Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 OHA, UK
Justin R. Crepp
Affiliation:
Department of Physics, University of Notre Dame, 225 Nieuwland Science Hall, Notre Dame, IN 46556, USA
John A. Johnson
Affiliation:
Department of Astronomy, California Institute of Technology, 1200 E. California Blvd., Pasadena, CA 91125, USA
Mark C. Wyatt
Affiliation:
Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 OHA, UK
Bruce Sibthorpe
Affiliation:
SRON Netherlands Institute for Space Research, Zernike Building, P.O. Box 800, 9700 AV Groningen, The Netherlands
Kate Y. L. Su
Affiliation:
Steward Observatory, University of Arizona, 933 N Cherry Ave., Tucson, AZ 85721
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Abstract

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Whilst debris discs orbiting main-sequence stars are well studied, very little is known regarding their fate when the star evolves onto the giant branch. For intermediate mass (A-type) stars, giants provide a unique opportunity to detect planets using the radial velocity technique, otherwise prohibited by high jitter levels and rotationally broadened lines in main-sequence intermediate mass (A-type) stars. Such stars can provide key insights into the structure of planetary systems around intermediate mass stars. In our Herschel OT1 program (PI Bonsor) we searched for the presence of debris discs orbiting a sample of 36 subgiants, half of which have RV detected companions. Our best detection is the resolved debris disc orbiting κ CrB.

Type
Contributed Papers
Copyright
Copyright © International Astronomical Union 2013 

References

Bonsor, A., Kennedy, G. M., Crepp, J. R., Johnson, J. A., Wyatt, M. C., Sibthorpe, B., & Su, K. Y. L. 2013, MNRAS 431 30253035CrossRefGoogle Scholar
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