The atmosphere and architecture of WASP-189 b probed by its CHEOPS phase curve

A. Deline; M. J. Hooton; M. Lendl; B. Morris; S. Salmon; G. Olofsson; C. Broeg; D. Ehrenreich; M. Beck; A. Brandeker; S. Hoyer; S. Sulis; V. Van Grootel; V. Bourrier; O. Demangeon; B.-O. Demory; K. Heng; H. Parviainen; L. M. Serrano; V. Singh; A. Bonfanti; L. Fossati; D. Kitzmann; S. G. Sousa; T. G. Wilson; Y. Alibert; R. Alonso; G. Anglada; T. Bárczy; D. Barrado Navascues; S. C. C. Barros; W. Baumjohann; T. Beck; A. Bekkelien; W. Benz; N. Billot; X. Bonfils; J. Cabrera; S. Charnoz; A. Collier Cameron; C. Corral van Damme; Sz. Csizmadia; M. B. Davies; M. Deleuil; L. Delrez; T. de Roche; A. Erikson; A. Fortier; M. Fridlund; D. Futyan; D. Gandolfi; M. Gillon; M. Güdel; P. Gutermann; J. Hasiba; K. G. Isaak; L. Kiss; J. Laskar; A. Lecavelier des Etangs; C. Lovis; D. Magrin; P. F. L. Maxted; M. Munari; V. Nascimbeni; R. Ottensamer; I. Pagano; E. Pallé; G. Peter; G. Piotto; D. Pollacco; D. Queloz; R. Ragazzoni; N. Rando; H. Rauer; I. Ribas; N. C. Santos; G. Scandariato; D. Ségransan; A. E. Simon; A. M. S. Smith; M. Steller; Gy. M. Szabó; N. Thomas; S. Udry; I. Walter; N. Walton

doi:10.1051/0004-6361/202142400

The atmosphere and architecture of WASP-189 b probed by its CHEOPS phase curve

A. Deline^*, M. J. Hooton, M. Lendl, B. Morris, S. Salmon, G. Olofsson, C. Broeg, D. Ehrenreich, M. Beck, A. Brandeker, S. Hoyer, S. Sulis, V. Van Grootel, V. Bourrier, O. Demangeon, B.-O. Demory, K. Heng, H. Parviainen, L. M. Serrano, V. SinghA. Bonfanti, L. Fossati, D. Kitzmann, S. G. Sousa, T. G. Wilson, Y. Alibert, R. Alonso, G. Anglada, T. Bárczy, D. Barrado Navascues, S. C. C. Barros, W. Baumjohann, T. Beck, A. Bekkelien, W. Benz, N. Billot, X. Bonfils, J. Cabrera, S. Charnoz, A. Collier Cameron, C. Corral van Damme, Sz. Csizmadia, M. B. Davies, M. Deleuil, L. Delrez, T. de Roche, A. Erikson, A. Fortier, M. Fridlund, D. Futyan, D. Gandolfi, M. Gillon, M. Güdel, P. Gutermann, J. Hasiba, K. G. Isaak, L. Kiss, J. Laskar, A. Lecavelier des Etangs, C. Lovis, D. Magrin, P. F. L. Maxted, M. Munari, V. Nascimbeni, R. Ottensamer, I. Pagano, E. Pallé, G. Peter, G. Piotto, D. Pollacco, D. Queloz, R. Ragazzoni, N. Rando, H. Rauer, I. Ribas, N. C. Santos, G. Scandariato, D. Ségransan, A. E. Simon, A. M. S. Smith, M. Steller, Gy. M. Szabó, N. Thomas, S. Udry, I. Walter, N. Walton

^*Corresponding author for this work

Research output: Contribution to journal › Article › peer-review

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, R-p = 1.600_-0.016^+0.017R_J, with a precision of 1%, and the true orbital obliquity of the planetary system, ψ_P = 89.6 ± 1.2 deg (polar orbit). We detect no significant hotspot offset from the phase curve and obtain an eclipse depth of δ_ecl = 96.5_-5.9^+4.5 ppm, from which we derive an upper limit on the geometric albedo: A_g < 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 similar 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).

Original language	English
Article number	74
Number of pages	24
Journal	Astronomy and Astrophysics
Volume	659
Early online date	8 Mar 2022
DOIs	https://doi.org/10.1051/0004-6361/202142400
Publication status	Published - 8 Mar 2022

Keywords

Techniques: photometric
Planets and satellites: atmospheres
Planets and satellites: individual: WASP-189 b

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Deline_2022_AA_atmosphere-architecture-WASP-189b_CC
Copyright © A. Deline et al. 2022. Open Access article, published by EDP Sciences, under the terms of the Creative Commons Attribution License (https://creativecommons.org/licenses/by/4.0), which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited.
Final published version, 18.3 MBLicence: CC BY

https://arxiv.org/abs/2201.04518Licence: CC BY

AO2 - Professor Andrew Cameron: Project AO2 - Andrew Cameron
Cameron, A. C. (PI)
Science & Technology Facilities Council
1/04/21 → 31/03/24
Project: Standard
Astronomy at St Andrews 2018-2021: Astronomy at St Andrews 2018-2021
Jardine, M. M. (PI), Bonnell, I. A. (CoI), Cameron, A. C. (CoI), Cyganowski, C. J. (CoI), Dominik, M. (CoI), Helling, C. (CoI), Horne, K. D. (CoI), Scholz, A. (CoI), Tojeiro, R. (CoI), Weijmans, A.-M. (CoI), Wild, V. (CoI), Woitke, P. (CoI), Wood, K. (CoI) & Zhao, H. (CoI)
1/04/18 → 31/03/22
Project: Standard
Support for the PLATO Development: Support for the PLATO Development Phase 2017-2022: Planet candidate ranking and validation
Cameron, A. C. (PI)
Science & Technology Facilities Council
1/08/17 → 31/12/22
Project: Standard

The atmosphere and architecture of WASP-189 b probed by its CHEOPS phase curve (dataset)
Wilson, T. G. (Creator) & Cameron, A. C. (Creator), VizieR On-line Data Catalog, 2022
http://cdsarc.u-strasbg.fr/viz-bin/cat/J/A+A/659/A74
Dataset

Cite this

Deline, A., Hooton, M. J., Lendl, M., Morris, B., Salmon, S., Olofsson, G., Broeg, C., Ehrenreich, D., Beck, M., Brandeker, A., Hoyer, S., Sulis, S., Van Grootel, V., Bourrier, V., Demangeon, O., Demory, B.-O., Heng, K., Parviainen, H., Serrano, L. M., ... Walton, N. (2022). The atmosphere and architecture of WASP-189 b probed by its CHEOPS phase curve. Astronomy and Astrophysics, 659, Article 74. https://doi.org/10.1051/0004-6361/202142400

@article{7d594f70bf5b4953904a7e547b59c374,

title = "The atmosphere and architecture of WASP-189 b probed by its CHEOPS phase curve",

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, R-p = 1.600-0.016+0.017RJ, with a precision of 1%, and the true orbital obliquity of the planetary system, ψP = 89.6 ± 1.2 deg (polar orbit). We detect no significant hotspot offset from the phase curve and obtain an eclipse depth of δecl = 96.5-5.9+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 similar 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).",

keywords = "Techniques: photometric, Planets and satellites: atmospheres, Planets and satellites: individual: WASP-189 b",

author = "A. Deline and Hooton, {M. J.} and M. Lendl and B. Morris and S. Salmon and G. Olofsson and C. Broeg and D. Ehrenreich and M. Beck and A. Brandeker and S. Hoyer and S. Sulis and {Van Grootel}, V. and V. Bourrier and O. Demangeon and B.-O. Demory and K. Heng and H. Parviainen and Serrano, {L. M.} and V. Singh and A. Bonfanti and L. Fossati and D. Kitzmann and Sousa, {S. G.} and Wilson, {T. G.} and Y. Alibert and R. Alonso and G. Anglada and T. B{\'a}rczy and {Barrado Navascues}, D. and Barros, {S. C. C.} and W. Baumjohann and T. Beck and A. Bekkelien and W. Benz and N. Billot and X. Bonfils and J. Cabrera and S. Charnoz and {Collier Cameron}, A. and {Corral van Damme}, C. and Sz. Csizmadia and Davies, {M. B.} and M. Deleuil and L. Delrez and {de Roche}, T. and A. Erikson and A. Fortier and M. Fridlund and D. Futyan and D. Gandolfi and M. Gillon and M. G{\"u}del and P. Gutermann and J. Hasiba and Isaak, {K. G.} and L. Kiss and J. Laskar and {Lecavelier des Etangs}, A. and C. Lovis and D. Magrin and Maxted, {P. F. L.} and M. Munari and V. Nascimbeni and R. Ottensamer and I. Pagano and E. Pall{\'e} and G. Peter and G. Piotto and D. Pollacco and D. Queloz and R. Ragazzoni and N. Rando and H. Rauer and I. Ribas and Santos, {N. C.} and G. Scandariato and D. S{\'e}gransan and Simon, {A. E.} and Smith, {A. M. S.} and M. Steller and Szab{\'o}, {Gy. M.} and N. Thomas and S. Udry and I. Walter and N. Walton",

note = "Funding: This project has received funding from the European Research Council (ERC) under the European Union{\textquoteright}s Horizon 2020 research and innovation programme (project FOUR ACES, grant agreement No. 724427). 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). 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. P.Ma. acknowledges support from STFC research grant number ST/M001040/1.",

year = "2022",

month = mar,

day = "8",

doi = "10.1051/0004-6361/202142400",

language = "English",

volume = "659",

journal = "Astronomy and Astrophysics",

issn = "0004-6361",

publisher = "EDP SCIENCES S A",

}

Deline, A, Hooton, MJ, Lendl, M, Morris, B, Salmon, S, Olofsson, G, Broeg, C, Ehrenreich, D, Beck, M, Brandeker, A, Hoyer, S, Sulis, S, Van Grootel, V, Bourrier, V, Demangeon, O, Demory, B-O, Heng, K, Parviainen, H, Serrano, LM, Singh, V, Bonfanti, A, Fossati, L, Kitzmann, D, Sousa, SG, Wilson, TG, Alibert, Y, Alonso, R, Anglada, G, Bárczy, T, Barrado Navascues, D, Barros, SCC, Baumjohann, W, Beck, T, Bekkelien, A, Benz, W, Billot, N, Bonfils, X, Cabrera, J, Charnoz, S, Collier Cameron, A, Corral van Damme, C, Csizmadia, S, Davies, MB, Deleuil, M, Delrez, L, de Roche, T, Erikson, A, Fortier, A, Fridlund, M, Futyan, D, Gandolfi, D, Gillon, M, Güdel, M, Gutermann, P, Hasiba, J, Isaak, KG, Kiss, L, Laskar, J, Lecavelier des Etangs, A, Lovis, C, Magrin, D, Maxted, PFL, Munari, M, Nascimbeni, V, Ottensamer, R, Pagano, I, Pallé, E, Peter, G, Piotto, G, Pollacco, D, Queloz, D, Ragazzoni, R, Rando, N, Rauer, H, Ribas, I, Santos, NC, Scandariato, G, Ségransan, D, Simon, AE, Smith, AMS, Steller, M, Szabó, GM, Thomas, N, Udry, S, Walter, I & Walton, N 2022, 'The atmosphere and architecture of WASP-189 b probed by its CHEOPS phase curve', Astronomy and Astrophysics, vol. 659, 74. https://doi.org/10.1051/0004-6361/202142400

TY - JOUR

T1 - The atmosphere and architecture of WASP-189 b probed by its CHEOPS phase curve

AU - Deline, A.

AU - Hooton, M. J.

AU - Lendl, M.

AU - Morris, B.

AU - Salmon, S.

AU - Olofsson, G.

AU - Broeg, C.

AU - Ehrenreich, D.

AU - Beck, M.

AU - Brandeker, A.

AU - Hoyer, S.

AU - Sulis, S.

AU - Van Grootel, V.

AU - Bourrier, V.

AU - Demangeon, O.

AU - Demory, B.-O.

AU - Heng, K.

AU - Parviainen, H.

AU - Serrano, L. M.

AU - Singh, V.

AU - Bonfanti, A.

AU - Fossati, L.

AU - Kitzmann, D.

AU - Sousa, S. G.

AU - Wilson, T. G.

AU - Alibert, Y.

AU - Alonso, R.

AU - Anglada, G.

AU - Bárczy, T.

AU - Barrado Navascues, D.

AU - Barros, S. C. C.

AU - Baumjohann, W.

AU - Beck, T.

AU - Bekkelien, A.

AU - Benz, W.

AU - Billot, N.

AU - Bonfils, X.

AU - Cabrera, J.

AU - Charnoz, S.

AU - Collier Cameron, A.

AU - Corral van Damme, C.

AU - Csizmadia, Sz.

AU - Davies, M. B.

AU - Deleuil, M.

AU - Delrez, L.

AU - de Roche, T.

AU - Erikson, A.

AU - Fortier, A.

AU - Fridlund, M.

AU - Futyan, D.

AU - Gandolfi, D.

AU - Gillon, M.

AU - Güdel, M.

AU - Gutermann, P.

AU - Hasiba, J.

AU - Isaak, K. G.

AU - Kiss, L.

AU - Laskar, J.

AU - Lecavelier des Etangs, A.

AU - Lovis, C.

AU - Magrin, D.

AU - Maxted, P. F. L.

AU - Munari, M.

AU - Nascimbeni, V.

AU - Ottensamer, R.

AU - Pagano, I.

AU - Pallé, E.

AU - Peter, G.

AU - Piotto, G.

AU - Pollacco, D.

AU - Queloz, D.

AU - Ragazzoni, R.

AU - Rando, N.

AU - Rauer, H.

AU - Ribas, I.

AU - Santos, N. C.

AU - Scandariato, G.

AU - Ségransan, D.

AU - Simon, A. E.

AU - Smith, A. M. S.

AU - Steller, M.

AU - Szabó, Gy. M.

AU - Thomas, N.

AU - Udry, S.

AU - Walter, I.

AU - Walton, N.

N1 - Funding: 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). 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). 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. P.Ma. acknowledges support from STFC research grant number ST/M001040/1.

PY - 2022/3/8

Y1 - 2022/3/8

N2 - 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, R-p = 1.600-0.016+0.017RJ, with a precision of 1%, and the true orbital obliquity of the planetary system, ψP = 89.6 ± 1.2 deg (polar orbit). We detect no significant hotspot offset from the phase curve and obtain an eclipse depth of δecl = 96.5-5.9+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 similar 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).

AB - 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, R-p = 1.600-0.016+0.017RJ, with a precision of 1%, and the true orbital obliquity of the planetary system, ψP = 89.6 ± 1.2 deg (polar orbit). We detect no significant hotspot offset from the phase curve and obtain an eclipse depth of δecl = 96.5-5.9+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 similar 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).

KW - Techniques: photometric

KW - Planets and satellites: atmospheres

KW - Planets and satellites: individual: WASP-189 b

U2 - 10.1051/0004-6361/202142400

DO - 10.1051/0004-6361/202142400

M3 - Article

SN - 0004-6361

VL - 659

JO - Astronomy and Astrophysics

JF - Astronomy and Astrophysics

M1 - 74

ER -

The atmosphere and architecture of WASP-189 b probed by its CHEOPS phase curve

Abstract

Keywords

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Projects

AO2 - Professor Andrew Cameron: Project AO2 - Andrew Cameron

Astronomy at St Andrews 2018-2021: Astronomy at St Andrews 2018-2021

Support for the PLATO Development: Support for the PLATO Development Phase 2017-2022: Planet candidate ranking and validation

Datasets

The atmosphere and architecture of WASP-189 b probed by its CHEOPS phase curve (dataset)

Cite this