The GROUSE project. III. Ks-band observations of the thermal emission from WASP-33b

Mooij, E. de; Brogi, M.; Kok, R. de; Snellen, I.A.G.; Kenworthy, M.A.; Karjalainen, R. (2013)

Article / Letter to editor

Context. In recent years, day-side emission from about a dozen hot Jupiters has been detected through ground-based secondary eclipse observations in the near-infrared. These near-infrared observations are vital for determining the energy budgets of hot Jupiters, since they probe the planet's spectral energy distribution near its peak.
Aims: The aim of this work is to measure the K$_s$-band secondary eclipse depth of WASP-33b, the first planet discovered to transit an A-type star. This planet receives the highest level of irradiation of all transiting planets discovered to date. Furthermore, its host-star shows pulsations and is classified as a low-amplitude {$delta$} Scuti.
Methods: As part of our GROUnd-based Secondary Eclipse (GROUSE) project we have obtained observations of two separate secondary eclipses of WASP-33b in the K$_s$-band using the LIRIS instrument on the William Herschel Telescope (WHT). The telescope was significantly defocused to avoid saturation of the detector for this bright star (K ~{} 7.5). To increase the stability and the cadence of the observations, they were performed in staring mode. We collected a total of 5100 and 6900 frames for the first and the second night respectively, both with an average cadence of 3.3 s.
Results: On the second night the eclipse is detected at the 12 -{$σ$} level, with a measured eclipse depth of 0.244$_{-0.020}$$^{+0.027}$%. This eclipse depth corresponds to a brightness temperature of 3270$_{-160}$$^{+115}$ K. The measured brightness temperature on the second night is consistent with the expected equilibrium temperature for a planet with a very low albedo and a rapid re-radiation of the absorbed stellar light. For the other night the short out-of-eclipse baseline prevents good corrections for the stellar pulsations and systematic effects, which makes this dataset unreliable for eclipse depth measurements. This demonstrates the need of getting a sufficient out-of-eclipse baseline. Appendix A is available in electronic form at http://www.aanda.orgLight curves are only available at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/550/A54

• All authors: Mooij, E. de; Brogi, M.; Kok, R. de; Snellen, I.A.G.; Kenworthy, M.A.; Karjalainen, R.
• Editor(s): Mooij, E.; Kok, R.
• Date: 2013
• Journal: Astronomy & Astrophysics
• Volume: 550
• Pages: A54
• DOI: doi:10.1051/0004-6361/201219434
• Link: http://adsabs.harvard.edu/abs/2013A&A...550A..54D