Architecture of TOI-561 planetary system

G. Piotto; T. Zingales; L. Borsato; J. A. Egger; A. C.M. Correia; A. E. Simon; H. G. Florén; S. G. Sousa; P. F.L. Maxted; D. Nardiello; L. Malavolta; T. G. Wilson; Y. Alibert; V. Adibekyan; A. Bonfanti; R. Luque; N. C. Santos; M. J. Hooton; L. Fossati; A. M.S. Smith; S. Salmon; G. Lacedelli; R. Alonso; T. Bárczy; D. Barrado Navascues; S. C.C. Barros; W. Baumjohann; T. Beck; W. Benz; N. Billot; A. Brandeker; C. Broeg; M. Buder; A. Collier Cameron; Sz Csizmadia; P. E. Cubillos; M. B. Davies; M. Deleuil; A. Deline; O. D.S. Demangeon; B. O. Demory; A. Derekas; B. Edwards; D. Ehrenreich; A. Erikson; A. Fortier; M. Fridlund; D. Gandolfi; K. Gazeas; M. Gillon; M. Güdel; M. N. Günther; A. Heitzmann; Ch Helling; K. G. Isaak; L. L. Kiss; J. Korth; K. W.F. Lam; J. Laskar; A. Lecavelier Des Etangs; M. Lendl; P. Leonardi; D. Magrin; G. Mantovan; C. Mordasini; V. Nascimbeni; G. Olofsson; R. Ottensamer; I. Pagano; E. Pallé; G. Peter; R. Ottensamer; D. Pollacco; D. Queloz; R. Ragazzoni; N. Rando; F. Ratti; H. Rauer; I. Ribas; G. Scandariato; D. Ségransan; D. Sicilia; M. Stalport; S. Sulis; Gy M. Szabó; S. Udry; S. Ulmer-Moll; V. Van Grootel; J. Venturini; E. Villaver; N. A. Walton; J. N. Winn; S. Wolf

doi:10.1093/mnras/stae2440

Architecture of TOI-561 planetary system

G. Piotto
, T. Zingales
, L. Borsato
, J. A. Egger
, A. C.M. Correia
, A. E. Simon
, H. G. Florén
, S. G. Sousa
, P. F.L. Maxted
, D. Nardiello
, L. Malavolta
, T. G. Wilson
, Y. Alibert
, V. Adibekyan
, A. Bonfanti
, R. Luque
, N. C. Santos
, M. J. Hooton
, L. Fossati
, A. M.S. Smith

S. Salmon, G. Lacedelli, R. Alonso, T. Bárczy, D. Barrado Navascues, S. C.C. Barros, W. Baumjohann, T. Beck, W. Benz, N. Billot, A. Brandeker, C. Broeg, M. Buder, A. Collier Cameron, Sz Csizmadia, P. E. Cubillos, M. B. Davies, M. Deleuil, A. Deline, O. D.S. Demangeon, B. O. Demory, A. Derekas, B. Edwards, D. Ehrenreich, A. Erikson, A. Fortier, M. Fridlund, D. Gandolfi, K. Gazeas, M. Gillon, M. Güdel, M. N. Günther, A. Heitzmann, Ch Helling, K. G. Isaak, L. L. Kiss, J. Korth, K. W.F. Lam, J. Laskar, A. Lecavelier Des Etangs, M. Lendl, P. Leonardi, D. Magrin, G. Mantovan, C. Mordasini, V. Nascimbeni, G. Olofsson, R. Ottensamer, I. Pagano, E. Pallé, G. Peter, R. Ottensamer, D. Pollacco, D. Queloz, R. Ragazzoni, N. Rando, F. Ratti, H. Rauer, I. Ribas, G. Scandariato, D. Ségransan, D. Sicilia, M. Stalport, S. Sulis, Gy M. Szabó, S. Udry, S. Ulmer-Moll, V. Van Grootel, J. Venturini, E. Villaver, N. A. Walton, J. N. Winn, S. Wolf

Dipartimento di Fisica e Astronomia 'galileo Galilei'
University of Padova
INAF Osservatorio Astronomico di Padova
University of Bern
University of Coimbra
Center for Space and Habitability
Department of Astronomy
Stockholm University
Ipatimup Diagnósticos
Astrophysics Group
Keele University
University of Warwick
Space Research Institute
University of Chicago
Departamento de Fisica e Astronomia
University of Cambridge
DLR
University of Geneva
Instituto de Astrofisica de Canarias
Departamento de Astrofisica
Research Unit; CIBERNED and Universidad de La Laguna
Admatis Ltd.
Departamento de Astrofísica
ESAC campus
University of St Andrews
Istituto di Astrofisica e Planetologia Spaziali (IAPS)
Lund University
LAM
Eötvös Loránd University
SRON - Netherlands Institute for Space Research
University of Leiden
Department of Space
Onsala Space Observatory
Dipartimento di Fisica
University of Turin
Physics Department
University of Athens
Astrobiology Research Unit
University of Liège
Department of Astrophysics
University of Vienna
ESTEC - European Space Research and Technology Centre
Institute for Theoretical Physics and Computational Physics
Graz University of Technology
Konkoly Observatory
Institute of Physics
Division of Astrophysics
Lund Observatory
Sorbonne Univ.
Institut d’Astrophysique de Paris
Università di Trento
INAF Osservatorio Astrofisico di Catania
Institute of Optical Sensor Systems
Princeton University
Department of Physics
ETH Zurich
Institut fuer Geologische Wissenschaften
Free University of Berlin
Campus UAB
Institut d’Estudis Espacials de Catalunya (IEEC)
HUN-REN–ELTE Exoplanet Research Group

Résultats de recherche: Contribution à un journal › Article › Revue par des pairs

5 Citations (Scopus)

Résumé

We present new observations from CHEOPS (CHaracterising ExOPlanet Satellite) and TESS (Transiting Exoplanet Survey Satellite) to clarify the architecture of the planetary system hosted by the old Galactic thick disc star TOI-561. Our global analysis, which also includes previously published photometric and radial velocity data, incontrovertibly proves that TOI-561 is hosting at least four transiting planets with periods of 0.44 d (TOI-561 b), 10.8 d (TOI-561 c), 25.7 d (TOI-561 d), and 77.1 d (TOI-561 e) and a fifth non-transiting candidate, TOI-561f with a period of 433 d. The precise characterization of TOI-561's orbital architecture is interesting since old and metal-poor thick disc stars are less likely to host ultrashort-period super-Earths like TOI-561 b. The new period of planet -e is consistent with the value obtained using radial velocity alone and is now known to be 77.14399 ± 0.00025 d, thanks to the new CHEOPS and TESS transits. The new data allowed us to improve its radius (R_p = 2.517 ± 0.045 R_⊕ from 5 per cent to 2 per cent precision) and mass(M_p = 12.4 ± 1.4 M_?) estimates, implying a density of ρ_p = 0.778 ± 0.097 ρ_⊕. Thanks to recent TESS observations and the focused CHEOPS visit of the transit of TOI-561 e, a good candidate for exomoon searches, the planet's period is finally constrained, allowing us to predict transit times through 2030 with 20-min accuracy. We present an updated version of the internal structure of the four transiting planets. We finally performed a detailed stability analysis, which confirmed the long-term stability of the outer planet TOI-561 f.

langue originale	Anglais
Pages (de - à)	2763-2774
Nombre de pages	12
journal	Monthly Notices of the Royal Astronomical Society
Volume	535
Numéro de publication	3
Les DOIs	https://doi.org/10.1093/mnras/stae2440
état	Publié - 1 déc. 2024
Modification externe	Oui

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10.1093/mnras/stae2440

Contient cette citation

Piotto, G., Zingales, T., Borsato, L., Egger, J. A., Correia, A. C. M., Simon, A. E., Florén, H. G., Sousa, S. G., Maxted, P. F. L., Nardiello, D., Malavolta, L., Wilson, T. G., Alibert, Y., Adibekyan, V., Bonfanti, A., Luque, R., Santos, N. C., Hooton, M. J., Fossati, L., ... Wolf, S. (2024). Architecture of TOI-561 planetary system. Monthly Notices of the Royal Astronomical Society, 535(3), 2763-2774. https://doi.org/10.1093/mnras/stae2440

@article{686a9feb47104ef590db1a3a2f525f02,

title = "Architecture of TOI-561 planetary system",

abstract = "We present new observations from CHEOPS (CHaracterising ExOPlanet Satellite) and TESS (Transiting Exoplanet Survey Satellite) to clarify the architecture of the planetary system hosted by the old Galactic thick disc star TOI-561. Our global analysis, which also includes previously published photometric and radial velocity data, incontrovertibly proves that TOI-561 is hosting at least four transiting planets with periods of 0.44 d (TOI-561 b), 10.8 d (TOI-561 c), 25.7 d (TOI-561 d), and 77.1 d (TOI-561 e) and a fifth non-transiting candidate, TOI-561f with a period of 433 d. The precise characterization of TOI-561's orbital architecture is interesting since old and metal-poor thick disc stars are less likely to host ultrashort-period super-Earths like TOI-561 b. The new period of planet -e is consistent with the value obtained using radial velocity alone and is now known to be 77.14399 ± 0.00025 d, thanks to the new CHEOPS and TESS transits. The new data allowed us to improve its radius (Rp = 2.517 ± 0.045 R⊕ from 5 per cent to 2 per cent precision) and mass(Mp = 12.4 ± 1.4 M?) estimates, implying a density of ρp = 0.778 ± 0.097 ρ⊕. Thanks to recent TESS observations and the focused CHEOPS visit of the transit of TOI-561 e, a good candidate for exomoon searches, the planet's period is finally constrained, allowing us to predict transit times through 2030 with 20-min accuracy. We present an updated version of the internal structure of the four transiting planets. We finally performed a detailed stability analysis, which confirmed the long-term stability of the outer planet TOI-561 f.",

keywords = "ephemerides, planets and satellites: dynamical evolution and stability, planets and satellites: fundamental parameters, planets and satellites: interiors, techniques: photometric, techniques: radial velocities",

author = "G. Piotto and T. Zingales and L. Borsato and Egger, \{J. A.\} and Correia, \{A. C.M.\} and Simon, \{A. E.\} and Flor{\'e}n, \{H. G.\} and Sousa, \{S. G.\} and Maxted, \{P. F.L.\} and D. Nardiello and L. Malavolta and Wilson, \{T. G.\} and Y. Alibert and V. Adibekyan and A. Bonfanti and R. Luque and Santos, \{N. C.\} and Hooton, \{M. J.\} and L. Fossati and Smith, \{A. M.S.\} and S. Salmon and G. Lacedelli and R. Alonso and T. B{\'a}rczy and \{Barrado Navascues\}, D. and Barros, \{S. C.C.\} and W. Baumjohann and T. Beck and W. Benz and N. Billot and A. Brandeker and C. Broeg and M. Buder and Cameron, \{A. Collier\} and Sz Csizmadia and Cubillos, \{P. E.\} and Davies, \{M. B.\} and M. Deleuil and A. Deline and Demangeon, \{O. D.S.\} and Demory, \{B. O.\} and A. Derekas and B. Edwards and D. Ehrenreich and A. Erikson and A. Fortier and M. Fridlund and D. Gandolfi and K. Gazeas and M. Gillon and M. G{\"u}del and G{\"u}nther, \{M. N.\} and A. Heitzmann 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 M. Lendl and P. Leonardi and D. Magrin and G. Mantovan and C. Mordasini and V. Nascimbeni and G. Olofsson and R. Ottensamer and I. Pagano and E. Pall{\'e} and G. Peter and R. Ottensamer and D. Pollacco and D. Queloz and R. Ragazzoni and N. Rando and F. Ratti and H. Rauer and I. Ribas and G. Scandariato and D. S{\'e}gransan and D. Sicilia and M. Stalport and S. Sulis and Szab{\'o}, \{Gy M.\} and S. Udry and S. Ulmer-Moll and \{Van Grootel\}, V. and J. Venturini and E. Villaver and Walton, \{N. A.\} and Winn, \{J. N.\} and S. Wolf",

note = "Publisher Copyright: {\textcopyright} 2024 The Author(s). Published by Oxford University Press on behalf of Royal Astronomical Society.",

year = "2024",

month = dec,

day = "1",

doi = "10.1093/mnras/stae2440",

language = "English",

volume = "535",

pages = "2763--2774",

journal = "Monthly Notices of the Royal Astronomical Society",

issn = "0035-8711",

publisher = "Oxford University Press",

number = "3",

}

Piotto, G, Zingales, T, Borsato, L, Egger, JA, Correia, ACM, Simon, AE, Florén, HG, Sousa, SG, Maxted, PFL, Nardiello, D, Malavolta, L, Wilson, TG, Alibert, Y, Adibekyan, V, Bonfanti, A, Luque, R, Santos, NC, Hooton, MJ, Fossati, L, Smith, AMS, Salmon, S, Lacedelli, G, Alonso, R, Bárczy, T, Barrado Navascues, D, Barros, SCC, Baumjohann, W, Beck, T, Benz, W, Billot, N, Brandeker, A, Broeg, C, Buder, M, Cameron, AC, Csizmadia, S, Cubillos, PE, Davies, MB, Deleuil, M, Deline, A, Demangeon, ODS, Demory, BO, Derekas, A, Edwards, B, Ehrenreich, D, Erikson, A, Fortier, A, Fridlund, M, Gandolfi, D, Gazeas, K, Gillon, M, Güdel, M, Günther, MN, Heitzmann, A, Helling, C, Isaak, KG, Kiss, LL, Korth, J, Lam, KWF, Laskar, J, Lecavelier Des Etangs, A, Lendl, M, Leonardi, P, Magrin, D, Mantovan, G, Mordasini, C, Nascimbeni, V, Olofsson, G, Ottensamer, R, Pagano, I, Pallé, E, Peter, G, Ottensamer, R, Pollacco, D, Queloz, D, Ragazzoni, R, Rando, N, Ratti, F, Rauer, H, Ribas, I, Scandariato, G, Ségransan, D, Sicilia, D, Stalport, M, Sulis, S, Szabó, GM, Udry, S, Ulmer-Moll, S, Van Grootel, V, Venturini, J, Villaver, E, Walton, NA, Winn, JN & Wolf, S 2024, 'Architecture of TOI-561 planetary system', Monthly Notices of the Royal Astronomical Society, VOL. 535, Numéro 3, p. 2763-2774. https://doi.org/10.1093/mnras/stae2440

TY - JOUR

T1 - Architecture of TOI-561 planetary system

AU - Piotto, G.

AU - Zingales, T.

AU - Borsato, L.

AU - Egger, J. A.

AU - Correia, A. C.M.

AU - Simon, A. E.

AU - Florén, H. G.

AU - Sousa, S. G.

AU - Maxted, P. F.L.

AU - Nardiello, D.

AU - Malavolta, L.

AU - Wilson, T. G.

AU - Alibert, Y.

AU - Adibekyan, V.

AU - Bonfanti, A.

AU - Luque, R.

AU - Santos, N. C.

AU - Hooton, M. J.

AU - Fossati, L.

AU - Smith, A. M.S.

AU - Salmon, S.

AU - Lacedelli, G.

AU - Alonso, R.

AU - Bárczy, T.

AU - Barrado Navascues, D.

AU - Barros, S. C.C.

AU - Baumjohann, W.

AU - Beck, T.

AU - Benz, W.

AU - Billot, N.

AU - Brandeker, A.

AU - Broeg, C.

AU - Buder, M.

AU - Cameron, A. Collier

AU - Csizmadia, Sz

AU - Cubillos, P. E.

AU - Davies, M. B.

AU - Deleuil, M.

AU - Deline, A.

AU - Demangeon, O. D.S.

AU - Demory, B. O.

AU - Derekas, A.

AU - Edwards, B.

AU - Ehrenreich, D.

AU - Erikson, A.

AU - Fortier, A.

AU - Fridlund, M.

AU - Gandolfi, D.

AU - Gazeas, K.

AU - Gillon, M.

AU - Güdel, M.

AU - Günther, M. N.

AU - Heitzmann, A.

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 - Lendl, M.

AU - Leonardi, P.

AU - Magrin, D.

AU - Mantovan, G.

AU - Mordasini, C.

AU - Nascimbeni, V.

AU - Olofsson, G.

AU - Ottensamer, R.

AU - Pagano, I.

AU - Pallé, E.

AU - Peter, G.

AU - Ottensamer, R.

AU - Pollacco, D.

AU - Queloz, D.

AU - Ragazzoni, R.

AU - Rando, N.

AU - Ratti, F.

AU - Rauer, H.

AU - Ribas, I.

AU - Scandariato, G.

AU - Ségransan, D.

AU - Sicilia, D.

AU - Stalport, M.

AU - Sulis, S.

AU - Szabó, Gy M.

AU - Udry, S.

AU - Ulmer-Moll, S.

AU - Van Grootel, V.

AU - Venturini, J.

AU - Villaver, E.

AU - Walton, N. A.

AU - Winn, J. N.

AU - Wolf, S.

PY - 2024/12/1

Y1 - 2024/12/1

N2 - We present new observations from CHEOPS (CHaracterising ExOPlanet Satellite) and TESS (Transiting Exoplanet Survey Satellite) to clarify the architecture of the planetary system hosted by the old Galactic thick disc star TOI-561. Our global analysis, which also includes previously published photometric and radial velocity data, incontrovertibly proves that TOI-561 is hosting at least four transiting planets with periods of 0.44 d (TOI-561 b), 10.8 d (TOI-561 c), 25.7 d (TOI-561 d), and 77.1 d (TOI-561 e) and a fifth non-transiting candidate, TOI-561f with a period of 433 d. The precise characterization of TOI-561's orbital architecture is interesting since old and metal-poor thick disc stars are less likely to host ultrashort-period super-Earths like TOI-561 b. The new period of planet -e is consistent with the value obtained using radial velocity alone and is now known to be 77.14399 ± 0.00025 d, thanks to the new CHEOPS and TESS transits. The new data allowed us to improve its radius (Rp = 2.517 ± 0.045 R⊕ from 5 per cent to 2 per cent precision) and mass(Mp = 12.4 ± 1.4 M?) estimates, implying a density of ρp = 0.778 ± 0.097 ρ⊕. Thanks to recent TESS observations and the focused CHEOPS visit of the transit of TOI-561 e, a good candidate for exomoon searches, the planet's period is finally constrained, allowing us to predict transit times through 2030 with 20-min accuracy. We present an updated version of the internal structure of the four transiting planets. We finally performed a detailed stability analysis, which confirmed the long-term stability of the outer planet TOI-561 f.

AB - We present new observations from CHEOPS (CHaracterising ExOPlanet Satellite) and TESS (Transiting Exoplanet Survey Satellite) to clarify the architecture of the planetary system hosted by the old Galactic thick disc star TOI-561. Our global analysis, which also includes previously published photometric and radial velocity data, incontrovertibly proves that TOI-561 is hosting at least four transiting planets with periods of 0.44 d (TOI-561 b), 10.8 d (TOI-561 c), 25.7 d (TOI-561 d), and 77.1 d (TOI-561 e) and a fifth non-transiting candidate, TOI-561f with a period of 433 d. The precise characterization of TOI-561's orbital architecture is interesting since old and metal-poor thick disc stars are less likely to host ultrashort-period super-Earths like TOI-561 b. The new period of planet -e is consistent with the value obtained using radial velocity alone and is now known to be 77.14399 ± 0.00025 d, thanks to the new CHEOPS and TESS transits. The new data allowed us to improve its radius (Rp = 2.517 ± 0.045 R⊕ from 5 per cent to 2 per cent precision) and mass(Mp = 12.4 ± 1.4 M?) estimates, implying a density of ρp = 0.778 ± 0.097 ρ⊕. Thanks to recent TESS observations and the focused CHEOPS visit of the transit of TOI-561 e, a good candidate for exomoon searches, the planet's period is finally constrained, allowing us to predict transit times through 2030 with 20-min accuracy. We present an updated version of the internal structure of the four transiting planets. We finally performed a detailed stability analysis, which confirmed the long-term stability of the outer planet TOI-561 f.

KW - ephemerides

KW - planets and satellites: dynamical evolution and stability

KW - planets and satellites: fundamental parameters

KW - planets and satellites: interiors

KW - techniques: photometric

KW - techniques: radial velocities

U2 - 10.1093/mnras/stae2440

DO - 10.1093/mnras/stae2440

M3 - Article

AN - SCOPUS:85210285301

SN - 0035-8711

VL - 535

SP - 2763

EP - 2774

JO - Monthly Notices of the Royal Astronomical Society

JF - Monthly Notices of the Royal Astronomical Society

IS - 3

ER -

Architecture of TOI-561 planetary system

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