Deline, A. and Hooton, M. J. and Lendl, M. and Morris, B. and Salmon, S. and Kiss, L. László and Szabó M., Gyula (2022) The atmosphere and architecture of WASP-189 b probed by its CHEOPS phase curve. ASTRONOMY & ASTROPHYSICS, 659. ISSN 0004-6361
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Abstract
Context. Gas giants orbiting close to hot and massive early-type stars can reach dayside temperatures that are comparable to those of the coldest stars. These `ultra-hot Jupiters' have atmospheres made of ions and atomic species from molecular dissociation and feature strong day-to-night temperature gradients. Photometric observations at different orbital phases provide insights on the planet's atmospheric properties. Aims: We aim to analyse the photometric observations of WASP-189 acquired with the Characterising Exoplanet Satellite (CHEOPS) to derive constraints on the system architecture and the planetary atmosphere. Methods: We implemented a light-curve model suited for an asymmetric transit shape caused by the gravity-darkened photosphere of the fast-rotating host star. We also modelled the reflective and thermal components of the planetary flux, the effect of stellar oblateness and light-travel time on transit-eclipse timings, the stellar activity, and CHEOPS systematics. Results: From the asymmetric transit, we measure the size of the ultra-hot Jupiter WASP-189 b, Rp = 1.600−0.016+0.017 RJ, with a precision of 1%, and the true orbital obliquity of the planetary system, Ψp = 89.6 ± 1.2deg (polar orbit). We detect no significant hotspot offset from the phase curve and obtain an eclipse depth of δecl = 96.5−5.0+4.5 ppm, from which we derive an upper limit on the geometric albedo: Ag < 0.48. We also find that the eclipse depth can only be explained by thermal emission alone in the case of extremely inefficient energy redistribution. Finally, we attribute the photometric variability to the stellar rotation, either through superficial inhomogeneities or resonance couplings between the convective core and the radiative envelope. Conclusions: Based on the derived system architecture, we predict the eclipse depth in the upcoming Transiting Exoplanet Survey Satellite (TESS) observations to be up to ~165 ppm. High-precision detection of the eclipse in both CHEOPS and TESS passbands might help disentangle reflective and thermal contributions. We also expect the right ascension of the ascending node of the orbit to precess due to the perturbations induced by the stellar quadrupole moment J2 (oblateness). Raw and detrended light curves are only available at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (ftp://130.79.128.5) or via http://cdsarc.u-strasbg.fr/viz-bin/cat/J/A+A/659/A74
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| Additional Information: | Funding Agency and Grant Number: European Research Council (ERC) under the European Union [724427, 947634, 851555]; Swiss National Science Foundation (SNSF); Swiss National Science Foundation [PCEFP2_194576, PP00P2-190080]; CNES [837319]; FCT -Fundacao para a Ciencia e a Tecnologia; FEDER through COMPETE2020 -Programa Operacional Competitividade e Internacionalizacao [UID/FIS/04434/2019, UIDB/04434/2020, UIDP/04434/2020, PTDC/FIS-AST/32113/2017, POCI-01-0145-FEDER032113, PTDC/FIS-AST/28953/2017, POCI-01-0145-FEDER-028953, PTDC/FIS-AST/28987/2017, POCI-01-0145-FEDER-028987]; FCT [DL 57/2016/CP1364/CT0004]; CRT foundation [2018.2323]; FCT through FCT contract [CEECIND/00826/2018]; POPH/FSE; STFC [ST/R000824/1, ST/V000861/1]; UKSA [ST/R003203/1]; Spanish Ministry of Science and Innovation; European Regional Development Fund [ESP2016-80435-C2-1-R, ESP2016-80435-C2-2-R, PGC2018-098153B-C33, PGC2018-098153-B-C31, ESP2017-87676-C5-1-R, MDM-2017-0737]; Generalitat de Catalunya/CERCA programme; ESA [4000124370]; FCT through FCT contracts [IF/01312/2014/CP1215/CT0004]; Belgian Federal Science Policy Office (BELSPO); University of Liege through an ARC grant for Concerted Research Actions - Wallonia-Brussels Federation; Swedish National Space Agency [DNR 65/19, 174/18]; Region Ile de France; project Equip@Meso of the programme Investissements d'Avenir [ANR-10-EQPX-29-01]; STFC research grant [ST/M001040/1]; Simons Foundation [327127] Funding text: This project has received funding from the European Research Council (ERC) under the European Union's Horizon 2020 research and innovation programme (project FOUR ACES, grant agreement No. 724427). It has also been carried out in the frame of the National Centre for Competence in Research "PlanetS" supported by the Swiss National Science Foundation (SNSF). A.De. acknowledges the financial support of the SNSF. M.J.Ho. and Y.Al. acknowledge the support of the Swiss National Fund under grant 200020_172746. M.Le. acknowledges support from the Swiss National Science Foundation under grant No. PCEFP2_194576. S.Sa. has received funding from the European Research Council (ERC) under the European Unions Horizon 2020 research and innovation programme (project STAREX, grant agreement No. 833925). D.Eh. acknowledges support from the European Research Council (ERC) under the European Union's Horizon 2020 research and innovation programme (project FOUR ACES, grant agreement No. 724427). A.Br. was supported by the SNSA. S.Ho. gratefully acknowledges CNES funding through the grant 837319. V.V.Gr. is an F.R.S-FNRS Research Associate. V.Bo. acknowledges support from the European Research Council (ERC) under the European Union's Horizon 2020 research and innovation programme (project FOUR ACES, grant agreement No. 724427; project SPICE DUNE, grant agreement No. 947634, project SCORE, grant agreement no. 851555). O.De. acknowledges support by FCT -Fundacao para a Ciencia e a Tecnologia through national funds and by FEDER through COMPETE2020 -Programa Operacional Competitividade e Internacionalizacao by these grants: UID/FIS/04434/2019, UIDB/04434/2020, UIDP/04434/2020, PTDC/FIS-AST/32113/2017 and POCI-01-0145-FEDER032113, PTDC/FIS-AST/28953/2017 and POCI-01-0145-FEDER-028953, PTDC/FIS-AST/28987/2017 and POCI-01-0145-FEDER-028987, O.De. is supported in the form of work contract (DL 57/2016/CP1364/CT0004) funded by national funds through FCT. B.-O.De. acknowledges support from the Swiss National Science Foundation (PP00P2-190080). L.M.Se. gratefully acknowledges financial support from the CRT foundation under Grant No. 2018.2323 "Gaseous or rocky? Unveiling the nature of small worlds". S.G.So. acknowledges support from FCT through FCT contract No. CEECIND/00826/2018 and POPH/FSE (EC). T.G.Wi. and A.C.Ca. acknowledge support from STFC consolidated grant numbers ST/R000824/1 and ST/V000861/1, and UKSA grant ST/R003203/1. R.Al. acknowledges support from the Spanish Ministry of Science and Innovation and the European Regional Development Fund through grants ESP2016-80435-C2-1-R, ESP2016-80435-C2-2-R, PGC2018-098153B-C33, PGC2018-098153-B-C31, ESP2017-87676-C5-1-R, MDM-2017-0737 Unidad de Excelencia Maria de Maeztu-Centro de Astrobiologi-a (INTA-CSIC), as well as the support of the Generalitat de Catalunya/CERCA programme. The MOC activities have been supported by the ESA contract No. 4000124370. S.C.C.Ba. acknowledges support from FCT through FCT contracts No. IF/01312/2014/CP1215/CT0004. X.Bo. acknowledges his role as ESA-appointed CHEOPS science team member. M.De. acknowledges support by the CNES. The Belgian participation to CHEOPS has been supported by the Belgian Federal Science Policy Office (BELSPO) in the framework of the PRODEX Program, and by the University of Liege through an ARC grant for Concerted Research Actions financed by the Wallonia-Brussels Federation. L.De. is an F.R.S.-FNRS Postdoctoral Researcher. M.Fr. gratefully acknowledges the support of the Swedish National Space Agency (DNR 65/19, 174/18). D.Ga.; gratefully acknowledges financial support from the CRT foundation under Grant No. 2018.2323 "Gaseous or rocky? Unveiling the nature of small worlds". M.Gi. is an F.R.S.-FNRS Senior Research Associate. K.G.Is. is the ESA CHEOPS Project Scientist and is responsible for the ESA CHEOPS Guest Observers Programme. She does not participate in, or contribute to, the definition of the Guaranteed Time Programme of the CHEOPS mission through which observations described in this paper have been taken, nor to any aspect of target selection for the programme. J.La. acknowledges granted access to the HPC resources of MesoPSL financed by the Region Ile de France and the project Equip@Meso (reference ANR-10-EQPX-29-01) of the programme Investissements d'Avenir supervised by the Agence Nationale pour la Recherche. P.Ma. acknowledges support from STFC research grant number ST/M001040/1. D.Qu. acknowledges partial support by a grant from the Simons Foundation (PI Queloz, grant number 327127). I.Ri. acknowledges support from the Spanish Ministry of Science and Innovation and the European Regional Development Fund through grant PGC2018-098153B-C33, as well as the support of the Generalitat de Catalunya/CERCA programme. This work has made use of data from the European Space Agency (ESA) mission Gaia (https://www.cosmos.esa.int/gaia), processed by the Gaia Data Processing and Analysis Consortium (DPAC, https://www.cosmos.esa.int/web/gaia/dpac/consortium).Funding for the DPAC has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement. We thank the referee for the insightful comments that helped improve the quality of this work. |
| Uncontrolled Keywords: | Astrophysics - Solar and Stellar Astrophysics; techniques: photometric; Astrophysics - Earth and Planetary Astrophysics; planets and satellites: atmospheres; planets and satellites: individual: WASP-189 b; |
| Subjects: | Q Science / természettudomány > QB Astronomy, Astrophysics / csillagászat, asztrofizika |
| SWORD Depositor: | MTMT SWORD |
| Depositing User: | MTMT SWORD |
| Date Deposited: | 09 Nov 2022 14:35 |
| Last Modified: | 09 Nov 2022 14:35 |
| URI: | http://real.mtak.hu/id/eprint/153158 |
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