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The CHEOPS view on the climate of WASP-3 b

Fuente: arXiv

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Auteurs principaux:	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., Valdes, E. Meier, Singh, V., Swayne, M. I., Alibert, Y., Alonso, R., Bárczy, T., Navascues, D. Barrado, Barros, S. C. C., Baumjohann, W., Benz, W., Billot, N., Borsato, L., Brandeker, A., Broeg, C., Buder, M., Busch, M. -D., Cameron, A. Collier, Correia, A. C. M., Csizmadia, Sz., Davies, M. B., Deleuil, M., Deline, A., Delrez, L., Demangeon, O. D. S., 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, Ch., Isaak, K. G., Kiss, L. L., Korth, J., Lam, K. W. F., Laskar, J., Etangs, A. Lecavelier des, 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, N. C., Ségransan, D., Simon, A. E., Smith, A. M. S., Sousa, S. G., Stalport, M., Sulis, S., Szabó, Gy. M., Udry, S., Van Grootel, V., Venturini, J., Villaver, E., Walton, N. A.
Format:	Preprint
Publié:	2024
Sujets:	Earth and Planetary Astrophysics
Accès en ligne:	Acceder al recurso
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_version_	1866910737158373376
author	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. Valdes, E. Meier Singh, V. Swayne, M. I. Alibert, Y. Alonso, R. Bárczy, T. Navascues, D. Barrado Barros, S. C. C. Baumjohann, W. Benz, W. Billot, N. Borsato, L. Brandeker, A. Broeg, C. Buder, M. Busch, M. -D. Cameron, A. Collier Correia, A. C. M. Csizmadia, Sz. Davies, M. B. Deleuil, M. Deline, A. Delrez, L. Demangeon, O. D. S. 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, Ch. Isaak, K. G. Kiss, L. L. Korth, J. Lam, K. W. F. Laskar, J. Etangs, A. Lecavelier des 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, N. C. Ségransan, D. Simon, A. E. Smith, A. M. S. Sousa, S. G. Stalport, M. Sulis, S. Szabó, Gy. M. Udry, S. Van Grootel, V. Venturini, J. Villaver, E. Walton, N. A.
author_facet	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. Valdes, E. Meier Singh, V. Swayne, M. I. Alibert, Y. Alonso, R. Bárczy, T. Navascues, D. Barrado Barros, S. C. C. Baumjohann, W. Benz, W. Billot, N. Borsato, L. Brandeker, A. Broeg, C. Buder, M. Busch, M. -D. Cameron, A. Collier Correia, A. C. M. Csizmadia, Sz. Davies, M. B. Deleuil, M. Deline, A. Delrez, L. Demangeon, O. D. S. 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, Ch. Isaak, K. G. Kiss, L. L. Korth, J. Lam, K. W. F. Laskar, J. Etangs, A. Lecavelier des 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, N. C. Ségransan, D. Simon, A. E. Smith, A. M. S. Sousa, S. G. Stalport, M. Sulis, S. Szabó, Gy. M. Udry, S. Van Grootel, V. Venturini, J. Villaver, E. Walton, N. A.
contents	Hot Jupiters are giant planets subject to intense stellar radiation. The physical and chemical properties of their atmosphere makes them the most amenable targets for the atmospheric characterization. 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. 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 which constrain the emission contribution in the \cheops and TESS passbands to approximately a few dozens of 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 $\sim$0.2. WASP-3 b belongs to the group of ultra-hot Jupiters which are characterized by low Bond albedo (<0.3+-0.1), as predicted by different atmospheric models. On the other hand, it unexpectedly seems to efficiently recirculate the absorbed stellar energy, unlike similar highly irradiated planets. To explain this inconsistency, we propose that other energy recirculation mechanisms may be at play other than advection (for example, dissociation and recombination of H_2). Another possibility is that the observations in different bandpasses probe different atmospheric layers, making 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.
format	Preprint
id	arxiv_https___arxiv_org_abs_2409_16268
institution	arXiv
publishDate	2024
record_format	arxiv
spellingShingle	The CHEOPS view on the climate of WASP-3 b 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. Valdes, E. Meier Singh, V. Swayne, M. I. Alibert, Y. Alonso, R. Bárczy, T. Navascues, D. Barrado Barros, S. C. C. Baumjohann, W. Benz, W. Billot, N. Borsato, L. Brandeker, A. Broeg, C. Buder, M. Busch, M. -D. Cameron, A. Collier Correia, A. C. M. Csizmadia, Sz. Davies, M. B. Deleuil, M. Deline, A. Delrez, L. Demangeon, O. D. S. 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, Ch. Isaak, K. G. Kiss, L. L. Korth, J. Lam, K. W. F. Laskar, J. Etangs, A. Lecavelier des 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, N. C. Ségransan, D. Simon, A. E. Smith, A. M. S. Sousa, S. G. Stalport, M. Sulis, S. Szabó, Gy. M. Udry, S. Van Grootel, V. Venturini, J. Villaver, E. Walton, N. A. Earth and Planetary Astrophysics Hot Jupiters are giant planets subject to intense stellar radiation. The physical and chemical properties of their atmosphere makes them the most amenable targets for the atmospheric characterization. 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. 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 which constrain the emission contribution in the \cheops and TESS passbands to approximately a few dozens of 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 $\sim$0.2. WASP-3 b belongs to the group of ultra-hot Jupiters which are characterized by low Bond albedo (<0.3+-0.1), as predicted by different atmospheric models. On the other hand, it unexpectedly seems to efficiently recirculate the absorbed stellar energy, unlike similar highly irradiated planets. To explain this inconsistency, we propose that other energy recirculation mechanisms may be at play other than advection (for example, dissociation and recombination of H_2). Another possibility is that the observations in different bandpasses probe different atmospheric layers, making 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.
title	The CHEOPS view on the climate of WASP-3 b
topic	Earth and Planetary Astrophysics
url	https://arxiv.org/abs/2409.16268