2013/08/01 by D. Föhring, Dóra Föhring, V. S. Dhillon +6 · 36 citations
Physics and Astronomy · #Astro and Planetary Science #Astronomy #Astrophysics #Astrophysics and Star Formation Studies #Eclipse #Exoplanet #Flux (metallurgy) #Hot Jupiter #Light curve #Photometry (optics) #Physics #Planet #Stars #Stellar, planetary, and galactic studies #Telescope #astro-ph.EP
paper · pdf · doi:10.1093/mnras/stt1443
published in Monthly Notices of the Royal Astronomical Society 435(3), 2268-2273 (Oxford University Press) · 6 pages, 4 figures, Accepted by MNRAS
arxiv created 2013/08/01 · openalex publication_date 2013/08/30 · arxiv updated 2015/06/16 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
We present z′-band secondary eclipse photometry of the highly irradiated hot Jupiter WASP-12b using ULTRACAM on the 4.2 m William Herschel Telescope. We measure a decrease in flux of δ = 0.130 ± 0.013 per cent during the passage of the planet behind the star, which is significantly deeper than the previous measurement at this wavelength (0.082 ± 0.015 per cent). Our secondary eclipse is best fitted with a mid-eclipse phase, ϕ, that is compatible with a circular orbit ϕ = 0.501 ± 0.002, in agreement with previous results. In combination with existing data, our eclipse depth measurement allows us to constrain the characteristics of the planet's atmosphere, which is consistent with a carbon-rich model, with no evidence for a strong thermal inversion. If the difference in eclipse depth reported here compared to that of López-Morales et al. is of physical origin, as opposed to due to systematics, it may be caused by temporal variability in the flux, due to atmospheric dynamics.