The hot dayside and asymmetric transit of WASP-189b seen by CHEOPS
Creators: name: Lendl, M.
name: Csizmadia, Sz.
name: Deline, A.
name: Fossati, L.
name: Kitzmann, D.
name: Heng, K.
name: Hoyer, S.
name: Salmon, S.
name: Benz, W.
name: Broeg, C.
name: Ehrenreich, D.
name: Fortier, A.
name: Queloz, D.
name: Bonfanti, A.
name: Brandeker, A.
name: Cameron, A. Collier
name: Delrez, L.
name: Muñoz, A. Garcia
name: Hooton, M. J.
name: Maxted, P. F. L.
name: Morris, B. M.
name: Van Grootel, V.
name: Wilson, T. G.
name: Alibert, Y.
name: Alonso, R.
name: Asquier, J.
name: Bárczy, T. Bandy T.
name: Barrado, D.
name: Barros, S. C. C
name: Baumjohann, W.
name: Beck, M.
name: Beck, T.
name: Bekkelien, A.
name: Bergomi, M.
name: Billot, N.
name: Biondi, F.
name: Bonfils, X.
name: Bourrier, V.
name: Busch, M-D.
name: Cabrera, J.
name: Cessa, V.
name: Charnoz, S.
name: Chazelas, B.
name: Van Damme, C. Corral
name: Davies, M. B.
name: Deleuil, M.
name: Demangeon, O. D. S
name: Demory, B. -O.
name: Erikson, A.
name: Farinato, J.
name: Fridlund, M.
name: Futyan, D.
name: Gandolfi, D.
name: Gillon, M.
name: Guterman, P.
name: Hasiba, J.
name: Hernandez, E.
name: Isaak, K. G.
name: Kiss, L.
name: Kuntzer, T.
name: Etangs, A. Lecavelier des
name: Lüftinger, T.
name: Laskar, J.
name: Lovis, C.
name: Magrin, D.
name: Malvasio, L.
name: Marafatto, L.
name: Michaelis, H.
name: Munari, M.
name: Nascimbeni, V.
name: Olofsson, G.
name: Ottacher, H.
name: Ottensamer, R.
name: Pagano, I.
name: Pallé, E.
name: Peter, G.
name: Piazza, D.
name: Piotto, G.
name: Pollacco, D.
name: Ratti, F.
name: Rauer, H.
name: Ragazzoni, R.
name: Rando, N.
name: Ribas, I.
name: Rieder, M.
name: Rohlfs, R.
name: Safa, F.
name: Santos, N. C.
name: Scandariato, G.
name: Ségransan, D.
name: Simon, A. E.
name: Singh, V.
name: Smith, A. M. S.
name: Sordet, M.
name: Sousa, S. G.
name: Steller, M.
name: Szabó, Gy. M.
name: Thomas, N.
name: Tschentscher, M.
name: Udry, S.
name: Viotto, V.
name: Walter, I.
name: Walton, N. A.
name: Wildi, F.
name: Wolter, D.
Publisher: name: arXiv
Year: 2020
Subjects: subject: Earth and Planetary Astrophysics (astro-ph.EP)
subject: Instrumentation and Methods for Astrophysics (astro-ph.IM)
subject: Solar and Stellar Astrophysics (astro-ph.SR)
subject: FOS: Physical sciences
subject: FOS: Physical sciences

description: The CHEOPS space mission dedicated to exoplanet follow-up was launched in December 2019, equipped with the capacity to perform photometric measurements at the 20 ppm level. As CHEOPS carries out its observations in a broad optical passband, it can provide insights into the reflected light from exoplanets and constrain the short-wavelength thermal emission for the hottest of planets by observing occultations and phase curves. Here, we report the first CHEOPS observation of an occultation, namely, that of the hot Jupiter WASP-189b, a $M_P \approx 2 M_J$ planet orbiting an A-type star. We detected the occultation of WASP-189 b at high significance in individual measurements and derived an occultation depth of $dF = 87.9 \pm 4.3$ppm based on four occultations. We compared these measurements to model predictions and we find that they are consistent with an unreflective atmosphere heated to a temperature of $3435 \pm 27$K, when assuming inefficient heat redistribution. Furthermore, we present two transits of WASP-189b observed by CHEOPS. These transits have an asymmetric shape that we attribute to gravity darkening of the host star caused by its high rotation rate. We used these measurements to refine the planetary parameters, finding a $\sim25\%$ deeper transit compared to the discovery paper and updating the radius of WASP-189b to $1.619\pm0.021 R_J$. We further measured the projected orbital obliquity to be $λ= 86.4^{+2.9}_{-4.4}$deg, a value that is in good agreement with a previous measurement from spectroscopic observations, and derived a true obliquity of $Ψ= 85.4\pm4.3$deg. Finally, we provide reference values for the photometric precision attained by the CHEOPS satellite: for the V=6.6 mag star, and using a one-hour binning, we obtain a residual RMS between 10 and 17ppm on the individual light curves, and 5.7ppm when combining the four visits.
description: In press at Astronomy and Astrophysics