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

A C Cameron, K Horne, D James, A Penny, M Semel

Research output: Book/ReportBook


We present new results derived from high-resolution optical spectra of the tau 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 epsilon < 3.5 x 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 R-p, = 1.2 R-J, 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.

Original languageEnglish
PublisherUnknown Publisher
Number of pages3
Publication statusPublished - 2004


  • 51 PEGASI


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