Volume 637, May 2020
|Number of page(s)||11|
|Section||Planets and planetary systems|
|Published online||08 May 2020|
Optical phase curve of the ultra-hot Jupiter WASP-121b★
Observatoire de l’Université de Genève,
51 chemin des Maillettes,
2 Center for Space and Habitability, Universität Bern, Gesellschaftsstrasse 6, 3012 Bern, Switzerland
3 INAF – Osservatorio Astronomico di Padova, Vicolo dell’Osservatorio 5, 35122 Padova, Italy
4 Anton Pannekoek Institute for Astronomy, University of Amsterdam, Science Park 904, 1098 XH Amsterdam, The Netherlands
5 European Southern Observatory, Alonso de Córdova 3107, Vitacura, Región Metropolitana, Chile
6 Departamento de Matemática y Física Aplicadas, Universidad Católica de la Santísima Concepción, Alonso de Rivera 2850, Concepción, Chile
7 SETI Institute, Mountain View, CA 94043, USA
8 NASA Ames Research Center, Moffett Field, CA 94035, USA
9 Instituto de Astrofísica de Canarias (IAC), 38205 La Laguna, Tenerife, Spain
10 Departamento de Astrofísica, Universidad de La Laguna (ULL), 38206 La Laguna, Tenerife, Spain
11 Department of Physics and Kavli Institute for Astrophysics and Space Research, MIT, Cambridge, MA 02139, USA
12 Department of Earth, Atmospheric and Planetary Sciences, Massachusetts Institute of Technology, Cambridge, MA 02139, USA
13 Department of Aeronautics and Astronautics, MIT, 77 Massachusetts Avenue, Cambridge, MA 02139, USA
14 Leiden Observatory, Leiden University, Postbus 9513, 2300 RA Leiden, The Netherlands
Accepted: 13 February 2020
We present the analysis of TESS optical photometry of WASP-121b, which reveals the phase curve of this transiting ultra-hot Jupiter. Its hotspot is located at the sub-stellar point, showing inefficient heat transport from the dayside (2870 ± 50 K) to the nightside (<2500 K at 3σ) at the altitudes probed by TESS. The TESS eclipse depth, measured at the shortest wavelength to date for WASP-121b, confirms the strong deviation from blackbody planetary emission. Our atmospheric retrieval on the complete emission spectrum supports the presence of a temperature inversion, which can be explained by the presence of VO and possibly TiO and FeH. The strong planetary emission at short wavelengths could arise from an H− continuum.
Key words: planetary systems / planets and satellites: individual: WASP-121b / planets and satellites: atmospheres / techniques: photometric
The reduced light curve of WASP-121, phase-folded at the planet orbital period and binned (Fig. 2) is available at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (188.8.131.52) or via http://cdsarc.u-strasbg.fr/viz-bin/cat/J/A+A/637/A36
© ESO 2020
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