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Precise characterisation of HD 15337 with CHEOPS: a laboratory for planet formation and evolution

Fuente: arXiv

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Bibliographic Details
Main Authors:	Rosário, N. M., Demangeon, O. D. S., Barros, S. C. C., Gandolfi, D., Egger, J. A., Serrano, L. M., Osborn, H. P., Beck, M., Benz, W., Florén, H. -G., Guterman, P., Wilson, T. G., Alibert, Y., Fossati, L., Hooton, M. J., Delrez, L., Santos, N. C., Sousa, S. G., Bonfanti, A., Salmon, S., Adibekyan, V., Nigioni, A., Venturini, J., Alonso, R., Anglada, G., Asquier, J., Bárczy, T., Navascues, D. Barrado, Barragán, O., Baumjohann, W., Beck, T., Billot, N., Biondi, F., Bonfils, X., Borsato, L., Brandeker, A., Broeg, C., Cessa, V., Charnoz, S., Cameron, A. Collier, Csizmadia, Sz., Cubillos, P. E., Davies, M. B., Deleuil, M., Deline, A., Demory, B. -O., Ehrenreich, D., Erikson, A., Esposito, M., Fortier, A., Fridlund, M., Gillon, M., Güdel, M., Günther, M. N., Helling, Ch., Hoyer, S., Isaak, K. G., Kiss, L. L., Lam, K. W. F., Laskar, J., Etangs, A. Lecavelier des, Lendl, M., Luntzer, A., Magrin, D., Maxted, P. F. L., Mordasini, C., Nascimbeni, V., Olofsson, G., Osborne, H. L. M., Ottensamer, R., Pagano, I., Pallé, E., Peter, G., Piotto, G., Pollacco, D., Queloz, D., Ragazzoni, R., Rando, N., Rauer, H., Ribas, I., Scandariato, G., Ségransan, D., Simon, A. E., Smith, A. M. S., Stalport, M., Szabó, Gy. M., Thomas, N., Udry, S., Van Eylen, V., Van Grootel, V., Villaver, E., Walter, I., Walton, N. A.
Format:	Preprint
Published:	2024
Subjects:	Earth and Planetary Astrophysics
Online Access:	Acceder al recurso
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author	Rosário, N. M. Demangeon, O. D. S. Barros, S. C. C. Gandolfi, D. Egger, J. A. Serrano, L. M. Osborn, H. P. Beck, M. Benz, W. Florén, H. -G. Guterman, P. Wilson, T. G. Alibert, Y. Fossati, L. Hooton, M. J. Delrez, L. Santos, N. C. Sousa, S. G. Bonfanti, A. Salmon, S. Adibekyan, V. Nigioni, A. Venturini, J. Alonso, R. Anglada, G. Asquier, J. Bárczy, T. Navascues, D. Barrado Barragán, O. Baumjohann, W. Beck, T. Billot, N. Biondi, F. Bonfils, X. Borsato, L. Brandeker, A. Broeg, C. Cessa, V. Charnoz, S. Cameron, A. Collier Csizmadia, Sz. Cubillos, P. E. Davies, M. B. Deleuil, M. Deline, A. Demory, B. -O. Ehrenreich, D. Erikson, A. Esposito, M. Fortier, A. Fridlund, M. Gillon, M. Güdel, M. Günther, M. N. Helling, Ch. Hoyer, S. Isaak, K. G. Kiss, L. L. Lam, K. W. F. Laskar, J. Etangs, A. Lecavelier des Lendl, M. Luntzer, A. Magrin, D. Maxted, P. F. L. Mordasini, C. Nascimbeni, V. Olofsson, G. Osborne, H. L. M. Ottensamer, R. Pagano, I. Pallé, E. Peter, G. Piotto, G. Pollacco, D. Queloz, D. Ragazzoni, R. Rando, N. Rauer, H. Ribas, I. Scandariato, G. Ségransan, D. Simon, A. E. Smith, A. M. S. Stalport, M. Szabó, Gy. M. Thomas, N. Udry, S. Van Eylen, V. Van Grootel, V. Villaver, E. Walter, I. Walton, N. A.
author_facet	Rosário, N. M. Demangeon, O. D. S. Barros, S. C. C. Gandolfi, D. Egger, J. A. Serrano, L. M. Osborn, H. P. Beck, M. Benz, W. Florén, H. -G. Guterman, P. Wilson, T. G. Alibert, Y. Fossati, L. Hooton, M. J. Delrez, L. Santos, N. C. Sousa, S. G. Bonfanti, A. Salmon, S. Adibekyan, V. Nigioni, A. Venturini, J. Alonso, R. Anglada, G. Asquier, J. Bárczy, T. Navascues, D. Barrado Barragán, O. Baumjohann, W. Beck, T. Billot, N. Biondi, F. Bonfils, X. Borsato, L. Brandeker, A. Broeg, C. Cessa, V. Charnoz, S. Cameron, A. Collier Csizmadia, Sz. Cubillos, P. E. Davies, M. B. Deleuil, M. Deline, A. Demory, B. -O. Ehrenreich, D. Erikson, A. Esposito, M. Fortier, A. Fridlund, M. Gillon, M. Güdel, M. Günther, M. N. Helling, Ch. Hoyer, S. Isaak, K. G. Kiss, L. L. Lam, K. W. F. Laskar, J. Etangs, A. Lecavelier des Lendl, M. Luntzer, A. Magrin, D. Maxted, P. F. L. Mordasini, C. Nascimbeni, V. Olofsson, G. Osborne, H. L. M. Ottensamer, R. Pagano, I. Pallé, E. Peter, G. Piotto, G. Pollacco, D. Queloz, D. Ragazzoni, R. Rando, N. Rauer, H. Ribas, I. Scandariato, G. Ségransan, D. Simon, A. E. Smith, A. M. S. Stalport, M. Szabó, Gy. M. Thomas, N. Udry, S. Van Eylen, V. Van Grootel, V. Villaver, E. Walter, I. Walton, N. A.
contents	We aim to constrain the internal structure and composition of HD 15337 b and c, two short-period planets situated on opposite sides of the radius valley, using new transit photometry and radial velocity data. We acquire 6 new transit visits with the CHaracterising ExOPlanet Satellite (CHEOPS) and 32 new radial velocity measurements from the High Accuracy Radial Velocity Planet Searcher (HARPS) to improve the accuracy of the mass and radius estimates for both planets. We reanalyse light curves from TESS sectors 3 and 4 and analyse new data from sector 30, correcting for long-term stellar activity. Subsequently, we perform a joint fit of the TESS and CHEOPS light curves, and all available RV data from HARPS and the Planet Finder Spectrograph (PFS). Our model fits the planetary signals, the stellar activity signal and the instrumental decorrelation model for the CHEOPS data simultaneously. The stellar activity was modelled using a Gaussian-process regression on both the RV and activity indicators. We finally employ a Bayesian retrieval code to determine the internal composition and structure of the planets. We derive updated and highly precise parameters for the HD 15337 system. Our improved precision on the planetary parameters makes HD 15337 b one of the most precisely characterised rocky exoplanets, with radius and mass measurements achieving a precision better than 2\% and 7\%, respectively. We are able to improve the precision of the radius measurement of HD 15337 c to 3\%. Our results imply that the composition of HD 15337 b is predominantly rocky, while HD 15337 c exhibits a gas envelope with a mass of at least $0.01\ M_\oplus$.Our results lay the groundwork for future studies, which can further unravel the atmospheric evolution of these exoplanets and give new insights into their composition and formation history and the causes behind the radius gap.
format	Preprint
id	arxiv_https___arxiv_org_abs_2403_16621
institution	arXiv
publishDate	2024
record_format	arxiv
spellingShingle	Precise characterisation of HD 15337 with CHEOPS: a laboratory for planet formation and evolution Rosário, N. M. Demangeon, O. D. S. Barros, S. C. C. Gandolfi, D. Egger, J. A. Serrano, L. M. Osborn, H. P. Beck, M. Benz, W. Florén, H. -G. Guterman, P. Wilson, T. G. Alibert, Y. Fossati, L. Hooton, M. J. Delrez, L. Santos, N. C. Sousa, S. G. Bonfanti, A. Salmon, S. Adibekyan, V. Nigioni, A. Venturini, J. Alonso, R. Anglada, G. Asquier, J. Bárczy, T. Navascues, D. Barrado Barragán, O. Baumjohann, W. Beck, T. Billot, N. Biondi, F. Bonfils, X. Borsato, L. Brandeker, A. Broeg, C. Cessa, V. Charnoz, S. Cameron, A. Collier Csizmadia, Sz. Cubillos, P. E. Davies, M. B. Deleuil, M. Deline, A. Demory, B. -O. Ehrenreich, D. Erikson, A. Esposito, M. Fortier, A. Fridlund, M. Gillon, M. Güdel, M. Günther, M. N. Helling, Ch. Hoyer, S. Isaak, K. G. Kiss, L. L. Lam, K. W. F. Laskar, J. Etangs, A. Lecavelier des Lendl, M. Luntzer, A. Magrin, D. Maxted, P. F. L. Mordasini, C. Nascimbeni, V. Olofsson, G. Osborne, H. L. M. Ottensamer, R. Pagano, I. Pallé, E. Peter, G. Piotto, G. Pollacco, D. Queloz, D. Ragazzoni, R. Rando, N. Rauer, H. Ribas, I. Scandariato, G. Ségransan, D. Simon, A. E. Smith, A. M. S. Stalport, M. Szabó, Gy. M. Thomas, N. Udry, S. Van Eylen, V. Van Grootel, V. Villaver, E. Walter, I. Walton, N. A. Earth and Planetary Astrophysics We aim to constrain the internal structure and composition of HD 15337 b and c, two short-period planets situated on opposite sides of the radius valley, using new transit photometry and radial velocity data. We acquire 6 new transit visits with the CHaracterising ExOPlanet Satellite (CHEOPS) and 32 new radial velocity measurements from the High Accuracy Radial Velocity Planet Searcher (HARPS) to improve the accuracy of the mass and radius estimates for both planets. We reanalyse light curves from TESS sectors 3 and 4 and analyse new data from sector 30, correcting for long-term stellar activity. Subsequently, we perform a joint fit of the TESS and CHEOPS light curves, and all available RV data from HARPS and the Planet Finder Spectrograph (PFS). Our model fits the planetary signals, the stellar activity signal and the instrumental decorrelation model for the CHEOPS data simultaneously. The stellar activity was modelled using a Gaussian-process regression on both the RV and activity indicators. We finally employ a Bayesian retrieval code to determine the internal composition and structure of the planets. We derive updated and highly precise parameters for the HD 15337 system. Our improved precision on the planetary parameters makes HD 15337 b one of the most precisely characterised rocky exoplanets, with radius and mass measurements achieving a precision better than 2\% and 7\%, respectively. We are able to improve the precision of the radius measurement of HD 15337 c to 3\%. Our results imply that the composition of HD 15337 b is predominantly rocky, while HD 15337 c exhibits a gas envelope with a mass of at least $0.01\ M_\oplus$.Our results lay the groundwork for future studies, which can further unravel the atmospheric evolution of these exoplanets and give new insights into their composition and formation history and the causes behind the radius gap.
title	Precise characterisation of HD 15337 with CHEOPS: a laboratory for planet formation and evolution
topic	Earth and Planetary Astrophysics
url	https://arxiv.org/abs/2403.16621