The TRAPPIST survey of southern transiting planets. I. Thirty eclipses of the ultra-short period planet WASP-43 b

By M. Gillon, A. Triaud, Jon Fortney, B. Demory, E. Jehin, M. Lendl, Pierre Magain, P. Kabáth, D. Queloz, R. Alonso and 9 more. 2012

159 citations recorded by the source corpus.

We present twenty-three transit light curves and seven occultation light curves for the ultra-short period planet WASP -43 b, in addition to eight new measurements of the radial velocity of the star. Thanks to this extensive data set, we improve significantly t he parameters of the system. Notably, the largely improved precision on the stellar density (2.41± 0.08ρ⊙) combined with constraining the age to be younger than a Hubble time allows us to break the degeneracy of the stellar solution mentioned in the discovery paper. The resulting stellar mass and size are 0.717± 0.025 M⊙ and 0.667± 0.011 R⊙. Our deduced physical parameters for the planet are 2.034± 0.052 MJup and 1.036± 0.019 RJup. Taking into account its level of irradiation, the high dens ity of the planet favors an old age and a massive core. Our deduced orbital eccentricity, 0.0035 +0.0060 −0.0025 , is consistent with a fully circularized orbit. We detect th e emission of the planet at 2.09µm at better than 11-σ, the deduced occultation depth being 1560± 140 ppm. Our detection of the occultation at 1.19µm is marginal (790± 320 ppm) and more observations are needed to confirm it. We pla ce a 3-σ upper limit of 850 ppm on the depth of the occultation at∼0.9µm. Together, these results strongly favor a poor redistribu tion of the heat to the night-side of the planet, and marginally favor a model with no day-side temperature inversion.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/acf5613fce97f3679344bc6e5f985f80f07b9524

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In Astronomy and Astrophysics

1. N. Madhusudhan
2. Jon Fortney
3. A. Showman
4. M. Line
5. J. D'esert
6. H. Knutson
7. V. Parmentier
8. Sara Seager

Citations in the corpus

• A SYSTEMATIC RETRIEVAL ANALYSIS OF SECONDARY ECLIPSE SPECTRA. I. A COMPARISON OF ATMOSPHERIC RETRIEVAL TECHNIQUES (2013, background): “…(see e.g., Knutson et al. 2010) and ground-based instruments (Croll et al. 2010; Anderson et al. 2010; Gibson et al. 2010; Deming et al. 2012; Gillon et al. 2012 ), as well as higher resolution spectra such as Hubble Space Telescopes Wide Field Camera 3 (WFC3) (Berta et al. 2012; Swain et…”
• A PRECISE WATER ABUNDANCE MEASUREMENT FOR THE HOT JUPITER WASP-43b (2014, methodology): “We found that using the highest-precision ground-based secondary eclipse measurements (Gillon et al. 2012) did not significantly affect our results, so our final analysis incorporates data from HST and Spitzer only.”
• WASP-121 b: a hot Jupiter close to tidal disruption transiting an active F star (2015, methodology): “A preliminary analysis was performed to determine the correction factors (CF ) for our photometric errors, as described in Gillon et al. (2012).”
• INFERENCE OF INHOMOGENEOUS CLOUDS IN AN EXOPLANET ATMOSPHERE (2013, methodology): “In order to model these data, we use the Markov Chain Monte Carlo (MCMC) implementation presented in Gillon et al. (2012).”
• SPITZER PHASE CURVE CONSTRAINTS FOR WASP-43b AT 3.6 AND 4.5 μm (2016, methodology): “Gillon et al. (2012) obtained nearly two dozen groundbased transit light curves to improve the precision of many system parameters.”