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A Search for the Spectroscopic Signature of Hot Jupiters

Published online by Cambridge University Press:  26 May 2016

P. W. Lucas  and
P. F. Roche
P. W. Lucas
Affiliation:
University of Hertfordshire, College Lane, Hatfield AL10 9AB, UK
P. F. Roche
Affiliation:
University of Oxford, Astrohysics Dept, 1 Keble Road, Oxford 0X1 3RH, UK

Abstract

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We describe a method by which hot extrasolar planets close to their parent star may be directly detected through the signature of water vapour or methane in their infrared spectra, lying on top of the spectrum of the parent star. Upper limits derived from low resolution K band spectra of several ‘hot Jupiter’ systems are presented. We find no water vapour to 3-σ limits of between 1 part in 200 and 1 part in 600 for each star. Comparison with an initial model indicates that constraints can be set on the size, albedo, temperature and dust content of the planets.

Type
Part I: Discovery and study of extrasolar planets - current
Information
Symposium - International Astronomical Union , Volume 202: Planetary Systems in the Universe – Observation, Formation and Evolution , 2004 , pp. 81 - 83
Copyright
Copyright © Astronomical Society of the Pacific 2004 

References

Charbonneau, , Brown, , Latham, & Mayor, 1999, ApJ, 529, L45.CrossRefGoogle Scholar
Henry, , Marcy, , Butler, & Vogt, 2000, ApJ, 529, L41.CrossRefGoogle Scholar
Leggett, Geballe, Fan + SLOAN collaboration 2000, ApJ, 536, L35.CrossRefGoogle Scholar