Precise characterisation of HD 15337 with CHEOPS: A laboratory for planet formation and evolution
Artikel i vetenskaplig tidskrift, 2024
Context. The HD 15337 (TIC 120896927, TOI-402) system was observed by the Transiting Exoplanet Survey Satellite (TESS), revealing the presence of two short-period planets situated on opposite sides of the radius gap. This offers an excellent opportunity to study theories of formation and evolution, as well as to investigate internal composition and atmospheric evaporation.
Aims. We aim to constrain the internal structure and composition of two short-period planets situated on opposite sides of the radius valley: HD 15337 b and c. We use new transit photometry and radial velocity data.
Methods. We acquired 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 re-analysed the light curves from TESS sectors 3 and 4 and analysed new data from sector 30, correcting for long-term stellar activity. Subsequently, we performed a joint fit of the TESS and CHEOPS light curves, along with all available RV data from HARPS and the Planet Finder Spectrograph (PFS). Our model fit the planetary signals, stellar activity signal, and 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. Finally, we employed a Bayesian retrieval code to determine the internal composition and structure of the planets.
Results. We derived 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 were 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-circle plus.
Conclusions. Our results lay the groundwork for future studies, which can further unravel the atmospheric evolution of these exoplanets and offer new insights into their composition and formation history as well as the causes behind the radius gap.
Aims. We aim to constrain the internal structure and composition of two short-period planets situated on opposite sides of the radius valley: HD 15337 b and c. We use new transit photometry and radial velocity data.
Methods. We acquired 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 re-analysed the light curves from TESS sectors 3 and 4 and analysed new data from sector 30, correcting for long-term stellar activity. Subsequently, we performed a joint fit of the TESS and CHEOPS light curves, along with all available RV data from HARPS and the Planet Finder Spectrograph (PFS). Our model fit the planetary signals, stellar activity signal, and 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. Finally, we employed a Bayesian retrieval code to determine the internal composition and structure of the planets.
Results. We derived 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 were 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-circle plus.
Conclusions. Our results lay the groundwork for future studies, which can further unravel the atmospheric evolution of these exoplanets and offer new insights into their composition and formation history as well as the causes behind the radius gap.
techniques: photometric
stars: individual: TIC 12089692
stars: individual: TOI-402
planets and satellites: composition
stars: individual: HD 15337
techniques: radial velocities
Författare
N. M. Rosario
Universidade do Porto
O. D. S. Demangeon
Universidade do Porto
S. C. C. Barros
Universidade do Porto
D. Gandolfi
Universita degli Studi di Torino
J. A. Egger
Universität Bern
L. M. Serrano
Universita degli Studi di Torino
H. P. Osborn
Massachusetts Institute of Technology (MIT)
Universität Bern
M. Beck
Université de Genève
W. Benz
Universität Bern
H. -G. Floren
Stockholms universitet
P. Guterman
Aix-Marseille Université
Institut National des Sciences de l'Univers
T. G. Wilson
The University of Warwick
University of St Andrews
Y. Alibert
Universität Bern
L. Fossati
Österreichische Akademie der Wissenschaften
M. J. Hooton
University of Cambridge
L. Delrez
Universite de Liège
N. C. Santos
Universidade do Porto
S. G. Sousa
Universidade do Porto
A. Bonfanti
Österreichische Akademie der Wissenschaften
S. Salmon
Université de Genève
V. Adibekyan
Universidade do Porto
A. Nigioni
Université de Genève
J. Venturini
Université de Genève
R. Alonso
Instituto de Astrofísica de Canarias
Universidad de la Laguna
G. Anglada
Centre Tecnològic de Telecomunicacions de Catalunya (CTTC)
Consejo Superior de Investigaciones Científicas (CSIC)
J. Asquier
European Space Research and Technology Centre (ESA ESTEC)
T. Barczy
Admatis
D. Barrado Navascues
Consejo Superior de Investigaciones Científicas (CSIC)
O. Barragan
University of Oxford
W. Baumjohann
Österreichische Akademie der Wissenschaften
T. Beck
Universität Bern
N. Billot
Université de Genève
F. Biondi
Istituto nazionale di astrofisica (INAF)
Max-Planck-Gesellschaft
X. Bonfils
Université Grenoble Alpes
L. Borsato
Istituto nazionale di astrofisica (INAF)
A. Brandeker
Stockholms universitet
C. Broeg
Universität Bern
V. Cessa
Universität Bern
S. Charnoz
Université Paris Cité
A. Collier Cameron
University of St Andrews
Sz. Csizmadia
Deutsches Zentrums für Luft- und Raumfahrt (DLR)
P. E. Cubillos
Istituto nazionale di astrofisica (INAF)
Österreichische Akademie der Wissenschaften
M. B. Davies
Lunds universitet
M. Deleuil
Aix-Marseille Université
A. Deline
Université de Genève
B. -O. Demory
Universität Bern
D. Ehrenreich
Université de Genève
A. Erikson
Deutsches Zentrums für Luft- und Raumfahrt (DLR)
M. Esposito
Thüringer Landessternwarte Tautenburg
A. Fortier
Universität Bern
Malcolm Fridlund
Chalmers, Rymd-, geo- och miljövetenskap, Astronomi och plasmafysik
M. Gillon
Universite de Liège
M. Guedel
Universität Wien
M. N. Gunther
European Space Research and Technology Centre (ESA ESTEC)
Ch. Helling
Österreichische Akademie der Wissenschaften
S. Hoyer
Aix-Marseille Université
K. G. Isaak
European Space Research and Technology Centre (ESA ESTEC)
L. L. Kiss
Eötvös Loránd University (ELTE)
Konkoly Observatory
K. W. F. Lam
Deutsches Zentrums für Luft- und Raumfahrt (DLR)
J. Laskar
Sorbonne Université
A. Lecavelier des Etangs
Université Pierre et Marie Curie (UPMC)
M. Lendl
Université de Genève
A. Luntzer
Technische Universität Wien
D. Magrin
Istituto nazionale di astrofisica (INAF)
P. F. L. Maxted
Keele University
C. Mordasini
Universität Bern
V. Nascimbeni
Istituto nazionale di astrofisica (INAF)
G. Olofsson
Stockholms universitet
H. L. M. Osborne
University College London (UCL)
European Southern Observatory Santiago
R. Ottensamer
Universität Wien
I. Pagano
Istituto nazionale di astrofisica (INAF)
E. Palle
Instituto de Astrofísica de Canarias
Universidad de la Laguna
G. Peter
Deutsches Zentrums für Luft- und Raumfahrt (DLR)
G. Piotto
Istituto nazionale di astrofisica (INAF)
Università di Padova
D. Pollacco
The University of Warwick
D. Queloz
Eidgenössische Technische Hochschule Zürich (ETH)
University of Cambridge
R. Ragazzoni
Istituto nazionale di astrofisica (INAF)
Università di Padova
N. Rando
European Space Research and Technology Centre (ESA ESTEC)
H. Rauer
Freie Universität Berlin
Technische Universität Berlin
Deutsches Zentrums für Luft- und Raumfahrt (DLR)
I. Ribas
Consejo Superior de Investigaciones Científicas (CSIC)
Centre Tecnològic de Telecomunicacions de Catalunya (CTTC)
G. Scandariato
Istituto nazionale di astrofisica (INAF)
D. Segransan
Université de Genève
A. E. Simon
Universität Bern
A. M. S. Smith
Deutsches Zentrums für Luft- und Raumfahrt (DLR)
M. Stalport
Universite de Liège
Gy. M. Szabo
Eötvös Loránd University (ELTE)
N. Thomas
Universität Bern
S. Udry
Université de Genève
V. Van Eylen
University College London (UCL)
V. Van Grootel
Universite de Liège
E. Villaver
Instituto de Astrofísica de Canarias
I. Walter
Deutsches Zentrums für Luft- und Raumfahrt (DLR)
N. A. Walton
University of Cambridge
Astronomy and Astrophysics
0004-6361 (ISSN) 1432-0746 (eISSN)
Vol. 686 A282Ämneskategorier (SSIF 2011)
Astronomi, astrofysik och kosmologi
Den kondenserade materiens fysik
DOI
10.1051/0004-6361/202347759