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Detection of a transit by the planetary companion of HD 80606
Article first published online: 16 APR 2009
DOI: 10.1111/j.1745-3933.2009.00653.x
© 2009 The Authors. Journal compilation © 2009 RAS
Issue
Monthly Notices of the Royal Astronomical Society: Letters
Volume 396, Issue 1, pages L16–L20, June 2009
Additional Information
How to Cite
Fossey, S. J., Waldmann, I. P. and Kipping, D. M. (2009), Detection of a transit by the planetary companion of HD 80606. Monthly Notices of the Royal Astronomical Society: Letters, 396: L16–L20. doi: 10.1111/j.1745-3933.2009.00653.x
Publication History
- Issue published online: 28 MAY 2009
- Article first published online: 16 APR 2009
- Accepted 2009 March 10. Received 2009 March 9; in original form 2009 February 26
- Abstract
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Keywords:
- techniques: photometric;
- occultations;
- planets and satellites: general;
- stars: individual: HD 80606;
- planetary systems
ABSTRACT
We report the detection of a transit egress by the ∼3.9-Jupiter-mass planet HD 80606b, an object in a highly eccentric orbit (e∼ 0.93) about its parent star of approximately solar type. The astrophysical reality of the signal of variability in HD 80606 is confirmed by observation with two independent telescope systems and checks against several reference stars in the field. Differential photometry with respect to the nearby comparison star HD 80607 provides a precise light curve. Modelling of the light curve with a full eccentric-orbit model indicates a planet/star-radius ratio of 0.1057 ± 0.0018, corresponding to a planet radius of 1.029 RJ for a solar-radius parent star; and a precise orbital inclination of 
, giving a total transit duration of 12.1 ± 0.4 hours. The planet hence joins HD 17156b in a class of highly eccentric transiting planets, in which HD 80606b has both the longest period and most eccentric orbit. The recently reported discovery of a secondary eclipse of HD 80606b by the Spitzer Space Observatory permits a combined analysis with the mid-time of primary transit in which the orbital parameters of the system can be tightly constrained. We derive a transit ephemeris of Ttr= HJD (245 4876.344 ± 0.011) + (111.4277 ± 0.0032) ×E.