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τ Boo b: Not so bright, but just as heavy

Published online by Cambridge University Press:  26 May 2016

Andrew Collier Cameron ,
Keith Horne ,
David James ,
Alan Penny  and
Meir Semel
Andrew Collier Cameron
Affiliation:
School of Physics and Astronomy, University of St Andrews, North Haugh, St Andrews, Fife KYI6 9SS, Scotland, UK
Keith Horne
Affiliation:
School of Physics and Astronomy, University of St Andrews, North Haugh, St Andrews, Fife KYI6 9SS, Scotland, UK
David James
Affiliation:
School of Physics and Astronomy, University of St Andrews, North Haugh, St Andrews, Fife KYI6 9SS, Scotland, UK
Alan Penny
Affiliation:
Rutherford Appleton Laboratory, Chilton, Didcot 0×11 0QX, UK
Meir Semel
Affiliation:
DAS OP, Observatoire de Paris-Meudon, F-92195 Meudon-Cedex, France

Abstract

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We present new results derived from high-resolution optical spectra of the τ Boo system, secured in March-May 2000. The results do not show the same feature reported by Cameron et al (1999) as a candidate reflected-light signature from the planet. Together with earlier results from the 1998 and 1999 seasons, the new data yield a 99.9% upper limit on the opposition planet/star flux ratio ∊ < 3.5 × 10−5 between 387.4 and 586.3 nm, a factor 3 deeper than the upper limit of Charbonneau et al (1999). For an assumed planet radius Rp = 1.2RJ, the upper limit on the mean geometric albedo is p < 0.22, 40% that of Jupiter. We find new evidence that the star's rotation is synchronised with the planet's orbital motion. Using a Monte Carlo analysis we infer that the planet's mass must lie in the range 5.5 to 10 times the mass of Jupiter.

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. 75 - 77
Copyright
Copyright © Astronomical Society of the Pacific 2004 

References

Baliunas, S. L., et al. 1998, ApJ, 474, L119.Google Scholar
Butler, R. P., et al. 1997, ApJ, 474, L115.Google Scholar
Burrows, A., et al. 2000, ApJ, 534, L97.Google Scholar
Cameron, A.C., Horne, K., Penny, A. J., James, D. J. 1999, Nature, 402, 751.Google Scholar
Charbonneau, D., et al. 1999, ApJ, 522, L145.Google Scholar
Fuhrmann, K., Pfeiffer, M. J., Bernkopf, J. 1998, A&A 336, 942.Google Scholar
Gonzalez, G. 1998, A&A, 334, 221.Google Scholar
Gray, D. F. 1982, ApJ, 258, 201.CrossRefGoogle Scholar
Marcy, G. W., et al. 1997, ApJ, 481, 926.CrossRefGoogle Scholar
Marley, M. S., et al. 1999, ApJ, 513, 879.Google Scholar
Seager, S., Sasselov, D. 1998, ApJ, 502, L157.CrossRefGoogle Scholar
Seager, S., Whitney, B., Sasselov, D. 2000, astro-ph 0004001.Google Scholar
Sudarsky, D., Burrows, A., Pinto, P. 2000, ApJ 538, 885.Google Scholar