{ "id": "astro-ph/0308413", "version": "v1", "published": "2003-08-23T14:51:00.000Z", "updated": "2003-08-23T14:51:00.000Z", "title": "A new upper limit on the reflected starlight from Tau Bootis b", "authors": [ "C. Leigh", "A. Collier Cameron", "K. Horne", "A. Penny", "D. James" ], "comment": "13 pages, 18 figures, MNRAS accepted 12 June 2003", "journal": "Mon.Not.Roy.Astron.Soc.344:1271,2003", "doi": "10.1046/j.1365-8711.2003.06901.x", "categories": [ "astro-ph" ], "abstract": "Using improved doppler tomographic signal-analysis techniques we have carried out a deep search for starlight reflected from the giant planet orbiting the star Tau 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 dataset comprises 893 high resolution spectra with a total integration time of 75 hr 32 min spanning 17 nights. We establish an upper limit on the planet's geometric albedo p<0.39 (at the 99.9 % significance level) at the most probable orbital inclination i=36 degrees, assuming a grey albedo, a Venus-like phase function and a planetary radius R_p=1.2 R_Jup. 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.", "revisions": [ { "version": "v1", "updated": "2003-08-23T14:51:00.000Z" } ], "analyses": { "keywords": [ "upper limit", "reflected starlight", "doppler tomographic signal-analysis techniques", "weak candidate signal appears", "planetary radius" ], "tags": [ "journal article" ], "note": { "typesetting": "TeX", "pages": 13, "language": "en", "license": "arXiv", "status": "editable", "inspire": 626477 } } }