The CHEOPS view on the climate of WASP-3 b

G. Scandariato; L. Carone; P. E. Cubillos; P. F. L. Maxted; T. Zingales; M. N. Günther; A. Heitzmann; M. Lendl; T. G. Wilson; A. Bonfanti; G. Bruno; A. Krenn; E. Meier Valdes; V. Singh; M. I. Swayne; Y. Alibert; R. Alonso; T. Bárczy; D. Barrado Navascues; S. C. C. Barros; W. Baumjohann; W. Benz; N. Billot; L. Borsato; A. Brandeker; C. Broeg; M. Buder; M. -D. Busch; A. Collier Cameron; A. C. M. Correia; Sz Csizmadia; M. B. Davies; M. Deleuil; A. Deline; L. Delrez; O. D. S. Demangeon; B. -O. Demory; A. Derekas; B. Edwards; D. Ehrenreich; A. Erikson; J. Farinato; A. Fortier; L. Fossati; M. Fridlund; D. Gandolfi; K. Gazeas; M. Gillon; M. Güdel; Ch Helling; K. G. Isaak; L. L. Kiss; J. Korth; K. W. F. Lam; J. Laskar; A. Lecavelier des Etangs; D. Magrin; B. Merín; C. Mordasini; V. Nascimbeni; G. Olofsson; R. Ottensamer; I. Pagano; E. Pallé; G. Peter; D. Piazza; G. Piotto; D. Pollacco; D. Queloz; R. Ragazzoni; N. Rando; H. Rauer; I. Ribas; N. C. Santos; D. Ségransan; A. E. Simon; A. M. S. Smith; S. G. Sousa; M. Stalport; S. Sulis; Gy M. Szabó; S. Udry; V. Van Grootel; J. Venturini; E. Villaver; N. A. Walton

doi:10.1051/0004-6361/202451049

The CHEOPS view on the climate of WASP-3 b

G. Scandariato^*, L. Carone, P. E. Cubillos, P. F. L. Maxted, T. Zingales, M. N. Günther, A. Heitzmann, M. Lendl, T. G. Wilson, A. Bonfanti, G. Bruno, A. Krenn, E. Meier Valdes, V. Singh, M. I. Swayne, Y. Alibert, R. Alonso, T. Bárczy, D. Barrado Navascues, S. C. C. BarrosW. Baumjohann, W. Benz, N. Billot, L. Borsato, A. Brandeker, C. Broeg, M. Buder, M. -D. Busch, A. Collier Cameron, A. C. M. Correia, Sz Csizmadia, M. B. Davies, M. Deleuil, A. Deline, L. Delrez, O. D. S. Demangeon, B. -O. Demory, A. Derekas, B. Edwards, D. Ehrenreich, A. Erikson, J. Farinato, A. Fortier, L. Fossati, M. Fridlund, D. Gandolfi, K. Gazeas, M. Gillon, M. Güdel, Ch Helling, K. G. Isaak, L. L. Kiss, J. Korth, K. W. F. Lam, J. Laskar, A. Lecavelier des Etangs, D. Magrin, B. Merín, C. Mordasini, V. Nascimbeni, G. Olofsson, R. Ottensamer, I. Pagano, E. Pallé, G. Peter, D. Piazza, G. Piotto, D. Pollacco, D. Queloz, R. Ragazzoni, N. Rando, H. Rauer, I. Ribas, N. C. Santos, D. Ségransan, A. E. Simon, A. M. S. Smith, S. G. Sousa, M. Stalport, S. Sulis, Gy M. Szabó, S. Udry, V. Van Grootel, J. Venturini, E. Villaver, N. A. Walton

^*Corresponding author for this work

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

Abstract

Context. Hot Jupiters are giant planets subject to intense stellar radiation. The physical and chemical properties of their atmosphere make them the most amenable targets for atmospheric characterization.
Aims. In this paper we analyze the photometry collected during the secondary eclipses of the hot Jupiter WASP-3 b by CHEOPS, TESS, and Spitzer. Our aim is to characterize the atmosphere of the planet by measuring the secondary eclipse depth in several passbands and constrain the planetary dayside spectrum.
Methods. We updated the radius and the ephemeris of WASP-3 b by analyzing the transit photometry collected by CHEOPS and TESS. We also analyzed the CHEOPS, TESS, and Spitzer photometry of the occultations of the planet, measuring the eclipse depth at different wavelengths.
Results. Our update of the stellar and planetary properties is consistent with previous works. The analysis of the occultations returns an eclipse depth of 92±21 ppm in the CHEOPS passband, 83±27 ppm for TESS, and >2000 ppm in the IRAC 1-2-4 Spitzer passbands. Using the eclipse depths in the Spitzer bands, we propose a set of likely emission spectra that constrain the emission contribution in the CHEOPS and TESS passbands to approximately a few dozen parts per million. This allowed us to measure a geometric albedo of 0.21±0.07 in the CHEOPS passband, while the TESS data lead to a 95% upper limit of ∼0.2.
Conclusions. WASP-3 b belongs to the group of ultra-hot Jupiters that are characterized by a low Bond albedo (<0.3±0.1), as predicted by different atmospheric models. On the other hand, it seems to efficiently recirculate the absorbed stellar energy, which is not typical for similar, highly irradiated planets. To explain this inconsistency, we propose that other energy recirculation mechanisms are at play besides advection (for example, the dissociation and recombination of H₂). Another possibility is that the observations in different bandpasses probe different atmospheric layers; this would make the atmospheric analysis difficult without an appropriate modeling of the thermal emission spectrum of WASP-3 b, which is not feasible with the limited spectroscopic data available to date.

Original language	English
Article number	A129
Number of pages	15
Journal	Astronomy & Astrophysics
Volume	692
Early online date	6 Dec 2024
DOIs	https://doi.org/10.1051/0004-6361/202451049
Publication status	Published - Dec 2024

Keywords

Techniques: photometric
Planets and satellites: atmospheres
Planets and satellites: detection
Planets and satellites: gaseous planets
Planets and satellites: individual: WASP-3b

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REVEAL: REVEALing Signatures of Habitable Worlds Hidden by Stellar Activity
Cameron, A. C. (PI)
UKRI (EU)
1/08/24 → 31/07/30
Project: Standard
AO2 - Professor Andrew Cameron: Project AO2 - Andrew Cameron
Cameron, A. C. (PI)
Science & Technology Facilities Council
1/04/21 → 31/03/24
Project: Standard
H2020 MSCA ITN EJD 2019: H2020 MSCA ITN EJD 2019 CHAMELEON
Helling, C. (PI)
European Commission
1/06/20 → 31/05/24
Project: Standard

The CHEOPS view on the climate of WASP-3 b (dataset)
Carone, L. A. (Creator), Cameron, A. C. (Creator) & Helling, C. (Creator), Centre de Donnees Strasbourg (CDS), 2024
https://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/692/A129
Dataset

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Scandariato, G., Carone, L., Cubillos, P. E., Maxted, P. F. L., Zingales, T., Günther, M. N., Heitzmann, A., Lendl, M., Wilson, T. G., Bonfanti, A., Bruno, G., Krenn, A., Meier Valdes, E., Singh, V., Swayne, M. I., Alibert, Y., Alonso, R., Bárczy, T., Barrado Navascues, D., ... Walton, N. A. (2024). The CHEOPS view on the climate of WASP-3 b. Astronomy & Astrophysics, 692, Article A129. https://doi.org/10.1051/0004-6361/202451049

@article{133af2fdaeac465cb3906a6852bd6d6c,

title = "The CHEOPS view on the climate of WASP-3 b",

abstract = "Context. Hot Jupiters are giant planets subject to intense stellar radiation. The physical and chemical properties of their atmosphere make them the most amenable targets for atmospheric characterization. Aims. In this paper we analyze the photometry collected during the secondary eclipses of the hot Jupiter WASP-3 b by CHEOPS, TESS, and Spitzer. Our aim is to characterize the atmosphere of the planet by measuring the secondary eclipse depth in several passbands and constrain the planetary dayside spectrum. Methods. We updated the radius and the ephemeris of WASP-3 b by analyzing the transit photometry collected by CHEOPS and TESS. We also analyzed the CHEOPS, TESS, and Spitzer photometry of the occultations of the planet, measuring the eclipse depth at different wavelengths. Results. Our update of the stellar and planetary properties is consistent with previous works. The analysis of the occultations returns an eclipse depth of 92±21 ppm in the CHEOPS passband, 83±27 ppm for TESS, and >2000 ppm in the IRAC 1-2-4 Spitzer passbands. Using the eclipse depths in the Spitzer bands, we propose a set of likely emission spectra that constrain the emission contribution in the CHEOPS and TESS passbands to approximately a few dozen parts per million. This allowed us to measure a geometric albedo of 0.21±0.07 in the CHEOPS passband, while the TESS data lead to a 95% upper limit of ∼0.2. Conclusions. WASP-3 b belongs to the group of ultra-hot Jupiters that are characterized by a low Bond albedo (<0.3±0.1), as predicted by different atmospheric models. On the other hand, it seems to efficiently recirculate the absorbed stellar energy, which is not typical for similar, highly irradiated planets. To explain this inconsistency, we propose that other energy recirculation mechanisms are at play besides advection (for example, the dissociation and recombination of H2). Another possibility is that the observations in different bandpasses probe different atmospheric layers; this would make the atmospheric analysis difficult without an appropriate modeling of the thermal emission spectrum of WASP-3 b, which is not feasible with the limited spectroscopic data available to date.",

keywords = "Techniques: photometric, Planets and satellites: atmospheres, Planets and satellites: detection, Planets and satellites: gaseous planets, Planets and satellites: individual: WASP-3b",

author = "G. Scandariato and L. Carone and Cubillos, {P. E.} and Maxted, {P. F. L.} and T. Zingales and G{\"u}nther, {M. N.} and A. Heitzmann and M. Lendl and Wilson, {T. G.} and A. Bonfanti and G. Bruno and A. Krenn and {Meier Valdes}, E. and V. Singh and Swayne, {M. I.} and Y. Alibert and R. Alonso and T. B{\'a}rczy and {Barrado Navascues}, D. and Barros, {S. C. C.} and W. Baumjohann and W. Benz and N. Billot and L. Borsato and A. Brandeker and C. Broeg and M. Buder and Busch, {M. -D.} and Cameron, {A. Collier} and Correia, {A. C. M.} and Sz Csizmadia and Davies, {M. B.} and M. Deleuil and A. Deline and L. Delrez and Demangeon, {O. D. S.} and Demory, {B. -O.} and A. Derekas and B. Edwards and D. Ehrenreich and A. Erikson and J. Farinato and A. Fortier and L. Fossati and M. Fridlund and D. Gandolfi and K. Gazeas and M. Gillon and M. G{\"u}del and Ch Helling and Isaak, {K. G.} and Kiss, {L. L.} and J. Korth and Lam, {K. W. F.} and J. Laskar and {Lecavelier des Etangs}, A. and D. Magrin and B. Mer{\'i}n and C. Mordasini and V. Nascimbeni and G. Olofsson and R. Ottensamer and I. Pagano and E. Pall{\'e} and G. Peter and D. Piazza 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 D. S{\'e}gransan and Simon, {A. E.} and Smith, {A. M. S.} and Sousa, {S. G.} and M. Stalport and S. Sulis and Szab{\'o}, {Gy M.} and S. Udry and {Van Grootel}, V. and J. Venturini and E. Villaver and Walton, {N. A.}",

note = "Funding: ACC acknowledges support from STFC consolidated grant number ST/V000861/1, and UKSA grant number ST/X002217/1. LCa and ChH acknowledge the European Union H2020-MSCA-ITN-2019 under Grant Agreement no. 860470 (CHAMELEON). PM acknowledges support from STFC research grant number ST/R000638/1. TWi acknowledges support from the UKSA and the University of Warwick. NCSa acknowledges funding by the European Union (ERC, FIERCE, 101052347). NAW acknowledges UKSA grant ST/R004838/1. ",

year = "2024",

month = dec,

doi = "10.1051/0004-6361/202451049",

language = "English",

volume = "692",

journal = "Astronomy & Astrophysics",

issn = "0004-6361",

publisher = "EDP SCIENCES S A",

}

Scandariato, G, Carone, L, Cubillos, PE, Maxted, PFL, Zingales, T, Günther, MN, Heitzmann, A, Lendl, M, Wilson, TG, Bonfanti, A, Bruno, G, Krenn, A, Meier Valdes, E, Singh, V, Swayne, MI, Alibert, Y, Alonso, R, Bárczy, T, Barrado Navascues, D, Barros, SCC, Baumjohann, W, Benz, W, Billot, N, Borsato, L, Brandeker, A, Broeg, C, Buder, M, Busch, M-D, Cameron, AC, Correia, ACM, Csizmadia, S, Davies, MB, Deleuil, M, Deline, A, Delrez, L, Demangeon, ODS, Demory, B-O, Derekas, A, Edwards, B, Ehrenreich, D, Erikson, A, Farinato, J, Fortier, A, Fossati, L, Fridlund, M, Gandolfi, D, Gazeas, K, Gillon, M, Güdel, M, Helling, C, Isaak, KG, Kiss, LL, Korth, J, Lam, KWF, Laskar, J, Lecavelier des Etangs, A, Magrin, D, Merín, B, Mordasini, C, Nascimbeni, V, Olofsson, G, Ottensamer, R, Pagano, I, Pallé, E, Peter, G, Piazza, D, Piotto, G, Pollacco, D, Queloz, D, Ragazzoni, R, Rando, N, Rauer, H, Ribas, I, Santos, NC, Ségransan, D, Simon, AE, Smith, AMS, Sousa, SG, Stalport, M, Sulis, S, Szabó, GM, Udry, S, Van Grootel, V, Venturini, J, Villaver, E & Walton, NA 2024, 'The CHEOPS view on the climate of WASP-3 b', Astronomy & Astrophysics, vol. 692, A129. https://doi.org/10.1051/0004-6361/202451049

TY - JOUR

T1 - The CHEOPS view on the climate of WASP-3 b

AU - Scandariato, G.

AU - Carone, L.

AU - Cubillos, P. E.

AU - Maxted, P. F. L.

AU - Zingales, T.

AU - Günther, M. N.

AU - Heitzmann, A.

AU - Lendl, M.

AU - Wilson, T. G.

AU - Bonfanti, A.

AU - Bruno, G.

AU - Krenn, A.

AU - Meier Valdes, E.

AU - Singh, V.

AU - Swayne, M. I.

AU - Alibert, Y.

AU - Alonso, R.

AU - Bárczy, T.

AU - Barrado Navascues, D.

AU - Barros, S. C. C.

AU - Baumjohann, W.

AU - Benz, W.

AU - Billot, N.

AU - Borsato, L.

AU - Brandeker, A.

AU - Broeg, C.

AU - Buder, M.

AU - Busch, M. -D.

AU - Cameron, A. Collier

AU - Correia, A. C. M.

AU - Csizmadia, Sz

AU - Davies, M. B.

AU - Deleuil, M.

AU - Deline, A.

AU - Delrez, L.

AU - Demangeon, O. D. S.

AU - Demory, B. -O.

AU - Derekas, A.

AU - Edwards, B.

AU - Ehrenreich, D.

AU - Erikson, A.

AU - Farinato, J.

AU - Fortier, A.

AU - Fossati, L.

AU - Fridlund, M.

AU - Gandolfi, D.

AU - Gazeas, K.

AU - Gillon, M.

AU - Güdel, M.

AU - Helling, Ch

AU - Isaak, K. G.

AU - Kiss, L. L.

AU - Korth, J.

AU - Lam, K. W. F.

AU - Laskar, J.

AU - Lecavelier des Etangs, A.

AU - Magrin, D.

AU - Merín, B.

AU - Mordasini, C.

AU - Nascimbeni, V.

AU - Olofsson, G.

AU - Ottensamer, R.

AU - Pagano, I.

AU - Pallé, E.

AU - Peter, G.

AU - Piazza, D.

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 - Ségransan, D.

AU - Simon, A. E.

AU - Smith, A. M. S.

AU - Sousa, S. G.

AU - Stalport, M.

AU - Sulis, S.

AU - Szabó, Gy M.

AU - Udry, S.

AU - Van Grootel, V.

AU - Venturini, J.

AU - Villaver, E.

AU - Walton, N. A.

N1 - Funding: ACC acknowledges support from STFC consolidated grant number ST/V000861/1, and UKSA grant number ST/X002217/1. LCa and ChH acknowledge the European Union H2020-MSCA-ITN-2019 under Grant Agreement no. 860470 (CHAMELEON). PM acknowledges support from STFC research grant number ST/R000638/1. TWi acknowledges support from the UKSA and the University of Warwick. NCSa acknowledges funding by the European Union (ERC, FIERCE, 101052347). NAW acknowledges UKSA grant ST/R004838/1.

PY - 2024/12

Y1 - 2024/12

N2 - Context. Hot Jupiters are giant planets subject to intense stellar radiation. The physical and chemical properties of their atmosphere make them the most amenable targets for atmospheric characterization. Aims. In this paper we analyze the photometry collected during the secondary eclipses of the hot Jupiter WASP-3 b by CHEOPS, TESS, and Spitzer. Our aim is to characterize the atmosphere of the planet by measuring the secondary eclipse depth in several passbands and constrain the planetary dayside spectrum. Methods. We updated the radius and the ephemeris of WASP-3 b by analyzing the transit photometry collected by CHEOPS and TESS. We also analyzed the CHEOPS, TESS, and Spitzer photometry of the occultations of the planet, measuring the eclipse depth at different wavelengths. Results. Our update of the stellar and planetary properties is consistent with previous works. The analysis of the occultations returns an eclipse depth of 92±21 ppm in the CHEOPS passband, 83±27 ppm for TESS, and >2000 ppm in the IRAC 1-2-4 Spitzer passbands. Using the eclipse depths in the Spitzer bands, we propose a set of likely emission spectra that constrain the emission contribution in the CHEOPS and TESS passbands to approximately a few dozen parts per million. This allowed us to measure a geometric albedo of 0.21±0.07 in the CHEOPS passband, while the TESS data lead to a 95% upper limit of ∼0.2. Conclusions. WASP-3 b belongs to the group of ultra-hot Jupiters that are characterized by a low Bond albedo (<0.3±0.1), as predicted by different atmospheric models. On the other hand, it seems to efficiently recirculate the absorbed stellar energy, which is not typical for similar, highly irradiated planets. To explain this inconsistency, we propose that other energy recirculation mechanisms are at play besides advection (for example, the dissociation and recombination of H2). Another possibility is that the observations in different bandpasses probe different atmospheric layers; this would make the atmospheric analysis difficult without an appropriate modeling of the thermal emission spectrum of WASP-3 b, which is not feasible with the limited spectroscopic data available to date.

AB - Context. Hot Jupiters are giant planets subject to intense stellar radiation. The physical and chemical properties of their atmosphere make them the most amenable targets for atmospheric characterization. Aims. In this paper we analyze the photometry collected during the secondary eclipses of the hot Jupiter WASP-3 b by CHEOPS, TESS, and Spitzer. Our aim is to characterize the atmosphere of the planet by measuring the secondary eclipse depth in several passbands and constrain the planetary dayside spectrum. Methods. We updated the radius and the ephemeris of WASP-3 b by analyzing the transit photometry collected by CHEOPS and TESS. We also analyzed the CHEOPS, TESS, and Spitzer photometry of the occultations of the planet, measuring the eclipse depth at different wavelengths. Results. Our update of the stellar and planetary properties is consistent with previous works. The analysis of the occultations returns an eclipse depth of 92±21 ppm in the CHEOPS passband, 83±27 ppm for TESS, and >2000 ppm in the IRAC 1-2-4 Spitzer passbands. Using the eclipse depths in the Spitzer bands, we propose a set of likely emission spectra that constrain the emission contribution in the CHEOPS and TESS passbands to approximately a few dozen parts per million. This allowed us to measure a geometric albedo of 0.21±0.07 in the CHEOPS passband, while the TESS data lead to a 95% upper limit of ∼0.2. Conclusions. WASP-3 b belongs to the group of ultra-hot Jupiters that are characterized by a low Bond albedo (<0.3±0.1), as predicted by different atmospheric models. On the other hand, it seems to efficiently recirculate the absorbed stellar energy, which is not typical for similar, highly irradiated planets. To explain this inconsistency, we propose that other energy recirculation mechanisms are at play besides advection (for example, the dissociation and recombination of H2). Another possibility is that the observations in different bandpasses probe different atmospheric layers; this would make the atmospheric analysis difficult without an appropriate modeling of the thermal emission spectrum of WASP-3 b, which is not feasible with the limited spectroscopic data available to date.

KW - Techniques: photometric

KW - Planets and satellites: atmospheres

KW - Planets and satellites: detection

KW - Planets and satellites: gaseous planets

KW - Planets and satellites: individual: WASP-3b

U2 - 10.1051/0004-6361/202451049

DO - 10.1051/0004-6361/202451049

M3 - Article

SN - 0004-6361

VL - 692

JO - Astronomy & Astrophysics

JF - Astronomy & Astrophysics

M1 - A129

ER -

The CHEOPS view on the climate of WASP-3 b

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Keywords

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Projects

REVEAL: REVEALing Signatures of Habitable Worlds Hidden by Stellar Activity

AO2 - Professor Andrew Cameron: Project AO2 - Andrew Cameron

H2020 MSCA ITN EJD 2019: H2020 MSCA ITN EJD 2019 CHAMELEON

Datasets

The CHEOPS view on the climate of WASP-3 b (dataset)

Cite this