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A new upper limit on the reflected starlight from  Bootis b

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Using improved Doppler tomographic signal-analysis techniques, we have carried out a deep search for starlight reflected from the giant planet orbiting the star  Bootis. We combined echelle spectra secured at the 4.2-m William Herschel telescope in 1998 and 1999 (which yielded a tentative detection of a reflected starlight component from the orbiting companion) with new data obtained in 2000 (which failed to confirm the detection). The combined data set comprises 893 high-resolution spectra with a total integration time of 75h 32m spanning 17 nights. We establish an upper limit on the planet's geometric albedo p < 0.39 (at the 99.9 per cent significance level) at the most probable orbital inclination i≃ 36° , assuming a grey albedo, a Venus-like phase function and a planetary radius Rp= 1.2RJup . We are able to rule out some combinations of the predicted planetary radius and atmospheric albedo models with high, reflective cloud decks. Although a weak candidate signal appears near to the most probable radial velocity amplitude, its statistical significance is insufficient for us to claim a detection with any confidence.
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Keywords: methods: data analysis; planetary systems; stars: individual:  Bootis; techniques: spectroscopic

Document Type: Research Article

Affiliations: 1: University of St Andrews, St Andrews, Fife, KY16 9SS 2: Rutherford Appleton Laboratory, Chilton, Didcot, Oxon, OX11 0QX 3: Observatoire de Grenoble, F-38041 Grenoble, Cedex 9, France

Publication date: October 1, 2003

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