Transit-timing variations in the AU Mic system observed with CHEOPS

Boldog; Gy M. Szabó; L. Kriskovics; L. Borsato; D. Gandolfi; M. Lendl; M. N. Günther; A. Heitzmann; T. G. Wilson; A. Brandeker; Z. Garai; Y. Alibert; R. Alonso; T. Bárczy; D. Barrado Navascues; S. C.C. Barros; W. Baumjohann; W. Benz; N. Billot; C. Broeg; A. Collier Cameron; A. C.M. Correia; Sz Csizmadia; P. E. Cubillos; M. B. Davies; M. Deleuil; A. Deline; O. D.S. Demangeon; B. O. Demory; A. Derekas; B. Edwards; J. A. Egger; D. Ehrenreich; A. Erikson; A. Fortier; L. Fossati; M. Fridlund; K. Gazeas; M. Gillon; M. Güdel; P. Guterman; Ch Helling; K. G. Isaak; L. L. Kiss; E. Kopp; J. Korth; K. W.F. Lam; J. Laskar; A. Lecavelier Des Etangs; A. Luntzer; D. Magrin; G. Mantovan; L. Marafatto; P. F.L. Maxted; B. Merín; C. Mordasini; M. Munari; V. Nascimbeni; G. Olofsson; R. Ottensamer; I. Pagano; E. Pallé; G. Peter; D. Piazza; G. Piotto; D. Pollacco; K. Poppenhaeger; D. Queloz; R. Ragazzoni; N. Rando; H. Rauer; I. Ribas; M. Rieder; N. C. Santos; G. Scandariato; D. Ségransan; A. E. Simon; A. M.S. Smith; S. G. Sousa; R. Southworth; M. Stalport; S. Sulis; S. Udry; S. Ulmer-Moll; V. Van Grootel; J. Venturini; E. Villaver; N. A. Walton; T. Zingales

doi:10.1051/0004-6361/202452699

Transit-timing variations in the AU Mic system observed with CHEOPS

Boldog
, Gy M. Szabó
, L. Kriskovics
, L. Borsato
, D. Gandolfi
, M. Lendl
, M. N. Günther
, A. Heitzmann
, T. G. Wilson
, A. Brandeker
, Z. Garai
, Y. Alibert
, R. Alonso
, T. Bárczy
, D. Barrado Navascues
, S. C.C. Barros
, W. Baumjohann
, W. Benz
, N. Billot
, C. Broeg

A. Collier Cameron, A. C.M. Correia, Sz Csizmadia, P. E. Cubillos, M. B. Davies, M. Deleuil, A. Deline, O. D.S. Demangeon, B. O. Demory, A. Derekas, B. Edwards, J. A. Egger, D. Ehrenreich, A. Erikson, A. Fortier, L. Fossati, M. Fridlund, K. Gazeas, M. Gillon, M. Güdel, P. Guterman, Ch Helling, K. G. Isaak, L. L. Kiss, E. Kopp, J. Korth, K. W.F. Lam, J. Laskar, A. Lecavelier Des Etangs, A. Luntzer, D. Magrin, G. Mantovan, L. Marafatto, P. F.L. Maxted, B. Merín, C. Mordasini, M. Munari, V. Nascimbeni, G. Olofsson, R. Ottensamer, I. Pagano, E. Pallé, G. Peter, D. Piazza, G. Piotto, D. Pollacco, K. Poppenhaeger, D. Queloz, R. Ragazzoni, N. Rando, H. Rauer, I. Ribas, M. Rieder, N. C. Santos, G. Scandariato, D. Ségransan, A. E. Simon, A. M.S. Smith, S. G. Sousa, R. Southworth, M. Stalport, S. Sulis, S. Udry, S. Ulmer-Moll, V. Van Grootel, J. Venturini, E. Villaver, N. A. Walton, T. Zingales

Konkoly Observatory
Mta Centre of Excellence
HUN-REN–ELTE Exoplanet Research Group
Eötvös Loránd University
INAF Osservatorio Astronomico di Padova
University of Turin
Université de Genève
ESTEC - European Space Research and Technology Centre
University of Warwick
Stockholm University
Astronomical Institute Slovak Academy of Sciences
University of Bern
University of Bern, Institute of Applied Physics
Instituto de Astrofisica de Canarias
Research Unit; CIBERNED and Universidad de La Laguna
Admatis Ltd.
ESAC campus
Ipatimup Diagnósticos
Space Research Institute
University of St Andrews
University of Coimbra
DLR
Istituto di Astrofisica e Planetologia Spaziali (IAPS)
Lund University
LAM
SRON - Netherlands Institute for Space Research
University of Geneva
University of Leiden
Onsala Space Observatory
University of Athens
University of Liège
University of Vienna
CS20330
Graz University of Technology
Lund Observatory
Sorbonne Univ.
Institut d’Astrophysique de Paris
University of Padova
Keele University
ESAC campus
INAF Osservatorio Astrofisico di Catania
Astrophysikalisches Institut Potsdam
ETH Zurich
University of Cambridge
Free University of Berlin
Campus UAB
Institut d’Estudis Espacials de Catalunya (IEEC)
European Space Agency / ESOC
Institute of Astronomy

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

Résumé

Context. AU Mic is a very active M dwarf star with an edge-on debris disk and two known transiting sub-Neptunes with a possible third planetary companion. The two transiting planets exhibit significant transit-timing variations (TTVs) that are caused by the gravi tational interaction between the bodies in the system. Aims. Using photometrical observations taken with the CHaracterizing ExOPlanet Satellite (CHEOPS), we aim to constrain the plan etary radii, the orbital distances, and the periods of AU Mic b and c. Furthermore, our goal is to determine the superperiod of the TTVs for AU Mic b and to update the transit ephemeris for both planets. Additionally, based on the perceived TTVs, we study the possible presence of a third planet in the system. Methods. We conducted ultra-high precision photometric observations with CHEOPS in 2022 and 2023. We used Allesfitter to fit the planetary transits and to constrain the planetary and orbital parameters. We combined our new measurements with results from previous years to determine the periods and amplitudes of the TTVs. We applied dynamical modelling based on TTV measurements from the 2018-2023 period to reconstruct the perceived variations. Results. We found that the orbital distances and periods for AU Mic b and c agree with the results from previous works. However, the values for the planetary radii deviate slightly from previous values, which we attribute to the effect of spots on the stellar surface. AU Mic c showed very strong TTVs, with transits that occurred ∼80 minutes later in 2023 than in 2021. Through a dynamical analysis of the system, we found that the observed TTVs can be explained by a third planet with an orbital period of ∼12.6 days and a mass of 0.203_0.024^+0.022 M_O. We explored the orbital geometry of the system and found that AU Mic c has a misaligned retrograde orbit. The limited number of AU Mic observations prevented us from determining the exact dynamical configuration and planetary parameters. Further monitoring of the system with CHEOPS might help to improve these results.

langue originale	Anglais
Numéro d'article	A137
journal	Astronomy and Astrophysics
Volume	694
Les DOIs	https://doi.org/10.1051/0004-6361/202452699
état	Publié - 1 févr. 2025
Modification externe	Oui

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10.1051/0004-6361/202452699

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Boldog, Szabó, G. M., Kriskovics, L., Borsato, L., Gandolfi, D., Lendl, M., Günther, M. N., Heitzmann, A., Wilson, T. G., Brandeker, A., Garai, Z., Alibert, Y., Alonso, R., Bárczy, T., Barrado Navascues, D., Barros, S. C. C., Baumjohann, W., Benz, W., Billot, N., ... Zingales, T. (2025). Transit-timing variations in the AU Mic system observed with CHEOPS. Astronomy and Astrophysics, 694, Article A137. https://doi.org/10.1051/0004-6361/202452699

@article{6230080d6ed14962a04cdae559f8515b,

title = "Transit-timing variations in the AU Mic system observed with CHEOPS",

abstract = "Context. AU Mic is a very active M dwarf star with an edge-on debris disk and two known transiting sub-Neptunes with a possible third planetary companion. The two transiting planets exhibit significant transit-timing variations (TTVs) that are caused by the gravi tational interaction between the bodies in the system. Aims. Using photometrical observations taken with the CHaracterizing ExOPlanet Satellite (CHEOPS), we aim to constrain the plan etary radii, the orbital distances, and the periods of AU Mic b and c. Furthermore, our goal is to determine the superperiod of the TTVs for AU Mic b and to update the transit ephemeris for both planets. Additionally, based on the perceived TTVs, we study the possible presence of a third planet in the system. Methods. We conducted ultra-high precision photometric observations with CHEOPS in 2022 and 2023. We used Allesfitter to fit the planetary transits and to constrain the planetary and orbital parameters. We combined our new measurements with results from previous years to determine the periods and amplitudes of the TTVs. We applied dynamical modelling based on TTV measurements from the 2018-2023 period to reconstruct the perceived variations. Results. We found that the orbital distances and periods for AU Mic b and c agree with the results from previous works. However, the values for the planetary radii deviate slightly from previous values, which we attribute to the effect of spots on the stellar surface. AU Mic c showed very strong TTVs, with transits that occurred ∼80 minutes later in 2023 than in 2021. Through a dynamical analysis of the system, we found that the observed TTVs can be explained by a third planet with an orbital period of ∼12.6 days and a mass of 0.2030.024+0.022 MO. We explored the orbital geometry of the system and found that AU Mic c has a misaligned retrograde orbit. The limited number of AU Mic observations prevented us from determining the exact dynamical configuration and planetary parameters. Further monitoring of the system with CHEOPS might help to improve these results.",

keywords = "Planets and satellites: fundamental parameters",

author = "Boldog and Szab{\'o}, \{Gy M.\} and L. Kriskovics and L. Borsato and D. Gandolfi and M. Lendl and G{\"u}nther, \{M. N.\} and A. Heitzmann and Wilson, \{T. G.\} and A. Brandeker and Z. Garai 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 C. Broeg and \{Collier Cameron\}, A. and Correia, \{A. C.M.\} 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 Egger, \{J. A.\} and D. Ehrenreich and A. Erikson and A. Fortier and L. Fossati and M. Fridlund and K. Gazeas and M. Gillon and M. G{\"u}del and P. Guterman and Ch Helling and Isaak, \{K. G.\} and Kiss, \{L. L.\} and E. Kopp and J. Korth and Lam, \{K. W.F.\} and J. Laskar and \{Lecavelier Des Etangs\}, A. and A. Luntzer and D. Magrin and G. Mantovan and L. Marafatto and Maxted, \{P. F.L.\} and B. Mer{\'i}n and C. Mordasini and M. Munari 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 K. Poppenhaeger and D. Queloz and R. Ragazzoni and N. Rando and H. Rauer and I. Ribas and M. Rieder and Santos, \{N. C.\} and G. Scandariato and D. S{\'e}gransan and Simon, \{A. E.\} and Smith, \{A. M.S.\} and Sousa, \{S. G.\} and R. Southworth and M. Stalport and S. Sulis and S. Udry and S. Ulmer-Moll and \{Van Grootel\}, V. and J. Venturini and E. Villaver and Walton, \{N. A.\} and T. Zingales",

note = "Publisher Copyright: {\textcopyright} The Authors 2025.",

year = "2025",

month = feb,

day = "1",

doi = "10.1051/0004-6361/202452699",

language = "English",

volume = "694",

journal = "Astronomy and Astrophysics",

issn = "0004-6361",

}

Boldog, Szabó, GM, Kriskovics, L, Borsato, L, Gandolfi, D, Lendl, M, Günther, MN, Heitzmann, A, Wilson, TG, Brandeker, A, Garai, Z, Alibert, Y, Alonso, R, Bárczy, T, Barrado Navascues, D, Barros, SCC, Baumjohann, W, Benz, W, Billot, N, Broeg, C, Collier Cameron, A, Correia, ACM, Csizmadia, S, Cubillos, PE, Davies, MB, Deleuil, M, Deline, A, Demangeon, ODS, Demory, BO, Derekas, A, Edwards, B, Egger, JA, Ehrenreich, D, Erikson, A, Fortier, A, Fossati, L, Fridlund, M, Gazeas, K, Gillon, M, Güdel, M, Guterman, P, Helling, C, Isaak, KG, Kiss, LL, Kopp, E, Korth, J, Lam, KWF, Laskar, J, Lecavelier Des Etangs, A, Luntzer, A, Magrin, D, Mantovan, G, Marafatto, L, Maxted, PFL, Merín, B, Mordasini, C, Munari, M, Nascimbeni, V, Olofsson, G, Ottensamer, R, Pagano, I, Pallé, E, Peter, G, Piazza, D, Piotto, G, Pollacco, D, Poppenhaeger, K, Queloz, D, Ragazzoni, R, Rando, N, Rauer, H, Ribas, I, Rieder, M, Santos, NC, Scandariato, G, Ségransan, D, Simon, AE, Smith, AMS, Sousa, SG, Southworth, R, Stalport, M, Sulis, S, Udry, S, Ulmer-Moll, S, Van Grootel, V, Venturini, J, Villaver, E, Walton, NA & Zingales, T 2025, 'Transit-timing variations in the AU Mic system observed with CHEOPS', Astronomy and Astrophysics, VOL. 694, A137. https://doi.org/10.1051/0004-6361/202452699

TY - JOUR

T1 - Transit-timing variations in the AU Mic system observed with CHEOPS

AU - Boldog,

AU - Szabó, Gy M.

AU - Kriskovics, L.

AU - Borsato, L.

AU - Gandolfi, D.

AU - Lendl, M.

AU - Günther, M. N.

AU - Heitzmann, A.

AU - Wilson, T. G.

AU - Brandeker, A.

AU - Garai, Z.

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 - Broeg, C.

AU - Collier Cameron, A.

AU - Correia, A. C.M.

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 - Egger, J. A.

AU - Ehrenreich, D.

AU - Erikson, A.

AU - Fortier, A.

AU - Fossati, L.

AU - Fridlund, M.

AU - Gazeas, K.

AU - Gillon, M.

AU - Güdel, M.

AU - Guterman, P.

AU - Helling, Ch

AU - Isaak, K. G.

AU - Kiss, L. L.

AU - Kopp, E.

AU - Korth, J.

AU - Lam, K. W.F.

AU - Laskar, J.

AU - Lecavelier Des Etangs, A.

AU - Luntzer, A.

AU - Magrin, D.

AU - Mantovan, G.

AU - Marafatto, L.

AU - Maxted, P. F.L.

AU - Merín, B.

AU - Mordasini, C.

AU - Munari, M.

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 - Poppenhaeger, K.

AU - Queloz, D.

AU - Ragazzoni, R.

AU - Rando, N.

AU - Rauer, H.

AU - Ribas, I.

AU - Rieder, M.

AU - Santos, N. C.

AU - Scandariato, G.

AU - Ségransan, D.

AU - Simon, A. E.

AU - Smith, A. M.S.

AU - Sousa, S. G.

AU - Southworth, R.

AU - Stalport, M.

AU - Sulis, S.

AU - Udry, S.

AU - Ulmer-Moll, S.

AU - Van Grootel, V.

AU - Venturini, J.

AU - Villaver, E.

AU - Walton, N. A.

AU - Zingales, T.

PY - 2025/2/1

Y1 - 2025/2/1

N2 - Context. AU Mic is a very active M dwarf star with an edge-on debris disk and two known transiting sub-Neptunes with a possible third planetary companion. The two transiting planets exhibit significant transit-timing variations (TTVs) that are caused by the gravi tational interaction between the bodies in the system. Aims. Using photometrical observations taken with the CHaracterizing ExOPlanet Satellite (CHEOPS), we aim to constrain the plan etary radii, the orbital distances, and the periods of AU Mic b and c. Furthermore, our goal is to determine the superperiod of the TTVs for AU Mic b and to update the transit ephemeris for both planets. Additionally, based on the perceived TTVs, we study the possible presence of a third planet in the system. Methods. We conducted ultra-high precision photometric observations with CHEOPS in 2022 and 2023. We used Allesfitter to fit the planetary transits and to constrain the planetary and orbital parameters. We combined our new measurements with results from previous years to determine the periods and amplitudes of the TTVs. We applied dynamical modelling based on TTV measurements from the 2018-2023 period to reconstruct the perceived variations. Results. We found that the orbital distances and periods for AU Mic b and c agree with the results from previous works. However, the values for the planetary radii deviate slightly from previous values, which we attribute to the effect of spots on the stellar surface. AU Mic c showed very strong TTVs, with transits that occurred ∼80 minutes later in 2023 than in 2021. Through a dynamical analysis of the system, we found that the observed TTVs can be explained by a third planet with an orbital period of ∼12.6 days and a mass of 0.2030.024+0.022 MO. We explored the orbital geometry of the system and found that AU Mic c has a misaligned retrograde orbit. The limited number of AU Mic observations prevented us from determining the exact dynamical configuration and planetary parameters. Further monitoring of the system with CHEOPS might help to improve these results.

AB - Context. AU Mic is a very active M dwarf star with an edge-on debris disk and two known transiting sub-Neptunes with a possible third planetary companion. The two transiting planets exhibit significant transit-timing variations (TTVs) that are caused by the gravi tational interaction between the bodies in the system. Aims. Using photometrical observations taken with the CHaracterizing ExOPlanet Satellite (CHEOPS), we aim to constrain the plan etary radii, the orbital distances, and the periods of AU Mic b and c. Furthermore, our goal is to determine the superperiod of the TTVs for AU Mic b and to update the transit ephemeris for both planets. Additionally, based on the perceived TTVs, we study the possible presence of a third planet in the system. Methods. We conducted ultra-high precision photometric observations with CHEOPS in 2022 and 2023. We used Allesfitter to fit the planetary transits and to constrain the planetary and orbital parameters. We combined our new measurements with results from previous years to determine the periods and amplitudes of the TTVs. We applied dynamical modelling based on TTV measurements from the 2018-2023 period to reconstruct the perceived variations. Results. We found that the orbital distances and periods for AU Mic b and c agree with the results from previous works. However, the values for the planetary radii deviate slightly from previous values, which we attribute to the effect of spots on the stellar surface. AU Mic c showed very strong TTVs, with transits that occurred ∼80 minutes later in 2023 than in 2021. Through a dynamical analysis of the system, we found that the observed TTVs can be explained by a third planet with an orbital period of ∼12.6 days and a mass of 0.2030.024+0.022 MO. We explored the orbital geometry of the system and found that AU Mic c has a misaligned retrograde orbit. The limited number of AU Mic observations prevented us from determining the exact dynamical configuration and planetary parameters. Further monitoring of the system with CHEOPS might help to improve these results.

KW - Planets and satellites: fundamental parameters

UR - https://www.scopus.com/pages/publications/85218126432

U2 - 10.1051/0004-6361/202452699

DO - 10.1051/0004-6361/202452699

M3 - Article

AN - SCOPUS:85218126432

SN - 0004-6361

VL - 694

JO - Astronomy and Astrophysics

JF - Astronomy and Astrophysics

M1 - A137

ER -

Transit-timing variations in the AU Mic system observed with CHEOPS

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