Characterisation of the warm-Jupiter TOI-1130 system with CHEOPS and photo-dynamical approach

L. Borsato; D. Degen; A. Leleu; M. J. Hooton; J. A. Egger; A. Bekkelien; A. Brandeker; A. Collier Cameron; M. N. Günther; V. Nascimbeni; C. M. Persson; A. Bonfanti; T. G. Wilson; A. C. M. Correia; T. Zingales; T. Guillot; A. H. M. J. Triaud; G. Piotto; D. Gandolfi; L. Abe; Y. Alibert; R. Alonso; T. Bárczy; D. Barrado Navascues; S. C. C. Barros; W. Baumjohann; T. Beck; P. Bendjoya; W. Benz; N. Billot; C. Broeg; M. -D. Busch; Sz Csizmadia; P. E. Cubillos; M. B. Davies; M. Deleuil; A. Deline; L. Delrez; O. D. S. Demangeon; B. -O. Demory; A. Derekas; B. Edwards; D. Ehrenreich; A. Erikson; A. Fortier; L. Fossati; M. Fridlund; K. Gazeas; M. Gillon; M. Güdel; A. Heitzmann; Ch Helling; S. Hoyer; K. G. Isaak; L. L. Kiss; J. Korth; K. W. F. Lam; J. Laskar; A. Lecavelier des Etangs; M. Lendl; D. Magrin; L. Marafatto; P. F. L. Maxted; M. Mecina; D. Mékarnia; C. Mordasini; D. Mura; G. Olofsson; R. Ottensamer; I. Pagano; E. Pallé; G. Peter; D. Pollacco; D. Queloz; R. Ragazzoni; N. Rando; F. Ratti; H. Rauer; I. Ribas; S. Salmon; N. C. Santos; G. Scandariato; D. Ségransan; A. E. Simon; A. M. S. Smith; S. G. Sousa; M. Stalport; O. Suarez; S. Sulis; Gy M. Szabó; S. Udry; V. Van Grootel; J. Venturini; E. Villaver; N. A. Walton; D. Wolter

doi:10.1051/0004-6361/202450974

Characterisation of the warm-Jupiter TOI-1130 system with CHEOPS and photo-dynamical approach

L. Borsato, D. Degen, A. Leleu, M. J. Hooton, J. A. Egger, A. Bekkelien, A. Brandeker, A. Collier Cameron, M. N. Günther, V. Nascimbeni, C. M. Persson, A. Bonfanti, T. G. Wilson, A. C. M. Correia, T. Zingales, T. Guillot, A. H. M. J. Triaud, G. Piotto, D. Gandolfi, L. AbeY. Alibert, R. Alonso, T. Bárczy, D. Barrado Navascues, S. C. C. Barros, W. Baumjohann, T. Beck, P. Bendjoya, W. Benz, N. Billot, C. Broeg, M. -D. Busch, Sz Csizmadia, P. E. Cubillos, M. B. Davies, M. Deleuil, A. Deline, L. Delrez, O. D. S. Demangeon, B. -O. Demory, A. Derekas, B. Edwards, D. Ehrenreich, A. Erikson, A. Fortier, L. Fossati, M. Fridlund, K. Gazeas, M. Gillon, M. Güdel, A. Heitzmann, Ch Helling, S. Hoyer, K. G. Isaak, L. L. Kiss, J. Korth, K. W. F. Lam, J. Laskar, A. Lecavelier des Etangs, M. Lendl, D. Magrin, L. Marafatto, P. F. L. Maxted, M. Mecina, D. Mékarnia, C. Mordasini, D. Mura, G. Olofsson, R. Ottensamer, I. Pagano, E. Pallé, G. Peter, D. Pollacco, D. Queloz, R. Ragazzoni, N. Rando, F. Ratti, H. Rauer, I. Ribas, S. Salmon, N. C. Santos, G. Scandariato, D. Ségransan, A. E. Simon, A. M. S. Smith, S. G. Sousa, M. Stalport, O. Suarez, S. Sulis, Gy M. Szabó, S. Udry, V. Van Grootel, J. Venturini, E. Villaver, N. A. Walton, D. Wolter

Research output: Contribution to journal › Article › peer-review

Abstract

Context. Among the thousands of exoplanets discovered to date, approximately a few hundred gas giants on short-period orbits are classified as ‘lonely’ and only a few are in a multi-planet system with a smaller companion on a close orbit. The processes that formed multi-planet systems hosting gas giants on close orbits are poorly understood, and only a few examples of this kind of system have been observed and well characterised.

Aims. Within the contest of a multi-planet system hosting a gas giant on short orbits, we characterise the TOI-1130 system by measuring masses and orbital parameters. This is a two-transiting planet system with a Jupiter-like planet (c) on a 8.35 days orbit and a Neptune-like planet (b) on an inner (4.07 days) orbit. Both planets show strong anti-correlated transit timing variations (TTVs). Furthermore, radial velocity (RV) analysis showed an additional linear trend, a possible hint of a non-transiting candidate planet on a far outer orbit.

Methods. Since 2019, extensive transit and radial velocity observations of the TOI-1130 have been acquired using TESS and various ground-based facilities. We present a new photo-dynamical analysis of all available transit and RV data, with the addition of new CHEOPS and ASTEP+ data, which achieve the best precision to date on the planetary radii and masses and on the timings of each transit.

Results. We were able to model interior structure of planet b constraining the presence of a gaseous envelope of H/He, while it was not possible to assess the possible water content. Furthermore, we analysed the resonant state of the two transiting planets, and we found that they lie just outside the resonant region. This could be the result of the tidal evolution that the system underwent. We obtained both masses of the planets with a precision of less than 1.5%, and radii with a precision of about 1% and 3% for planet b and c, respectively.

Original language	English
Article number	A52
Number of pages	21
Journal	Astronomy & Astrophysics
Volume	689
Early online date	3 Sept 2024
DOIs	https://doi.org/10.1051/0004-6361/202450974
Publication status	Published - Sept 2024

Keywords

Methods: data analysis
Methods: observational
Techniques: photometric
Telescopes
Planetary systems

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https://arxiv.org/abs/2407.06097Licence: CC BY-NC-SA

1 Active
2 Finished

REVEAL: REVEALing Signatures of Habitable Worlds Hidden by Stellar Activity
Cameron, A. (PI)
UKRI (EU)
1/08/24 → 31/07/30
Project: Standard
AO2 - Professor Andrew Cameron: Project AO2 - Andrew Cameron
Cameron, A. (PI)
Science & Technology Facilities Council
1/04/21 → 31/03/24
Project: Standard
H2020 MSCA ITN EJD 2019: H2020 MSCA ITN EJD 2019 CHAMELEON
Helling, C. (PI)
European Commission
1/06/20 → 31/05/24
Project: Standard

TOI-1130 CHEOPS observations
Borsato, L. (Creator), Degen, D. (Creator), Leleu, A. (Creator), Hooton, M. J. (Creator), Egger, J. A. (Creator), Bekkelien, A. (Creator), Brandeker, A. (Creator), Collier Cameron, A. (Creator), Guenther, M. N. (Creator), Nascimbeni, V. (Creator), Persson, C. M. (Creator), Bonfanti, A. (Creator), Wilson, T. G. (Creator), Correia, A. C. M. (Creator), Zingales, T. (Creator), Guillot, T. (Creator), Triaud, A. H. M. J. (Creator), Piotto, G. (Creator), Gandolfi, D. (Creator), Abe, L. (Creator), Alibert, Y. (Creator), Alonso, R. (Creator), Barczy, T. (Creator), Barrado Navascues, D. (Creator), Barros, S. C. C. (Creator), Baumjohann, W. (Creator), Beck, T. (Creator), Bendjoya, P. (Creator), Benz, W. (Creator), Billot, N. (Creator), Broeg, C. (Creator), Busch, M.-D. (Creator), Sz, C. (Creator), Cubillos, P. E. (Creator), Davies, M. B. (Creator), Deleuil, M. (Creator), Deline, A. (Creator), Delrez, L. (Creator), Demangeon, O. D. S. (Creator), Demory, B.-O. (Creator), Derekas, A. (Creator), Edwards, B. (Creator), Ehrenreich, D. (Creator), Erikson, A. (Creator), Fortier, A. (Creator), Fossati, L. (Creator), Fridlund, M. (Creator), Gazeas, K. (Creator), Gillon, M. (Creator), Guedel, M. (Creator), Heitzmann, A. (Creator), Helling, C. (Creator), Hoyer, S. (Creator), Isaak, K. G. (Creator), Kiss, L. L. (Creator), Korth, J. (Creator), K.W.F., L. (Creator), Laskar, J. (Creator), Lecavelier Des Etangs, A. (Creator), Lendl, M. (Creator), Magrin, D. (Creator), Marafatto, L. (Creator), Maxted, P. F. L. (Creator), Mecina, M. (Creator), Mekarnia, D. (Creator), Mordasini, C. (Creator), Mura, D. (Creator), Olofsson, G. (Creator), Ottensamer, R. (Creator), Pagano, I. (Creator), Palle, E. (Creator), Peter, G. (Creator), Pollacco, D. (Creator), Queloz, D. (Creator), Ragazzoni, R. (Creator), Rando, N. (Creator), Ratti, F. (Creator), Rauer, H. (Creator), Ribas, I. (Creator), Salmon, S. (Creator), Santos, N. C. (Creator), Scandariato, G. (Creator), Segransan, D. (Creator), Simon, A. E. (Creator), Smith, A. M. S. (Creator), Sousa, S. G. (Creator), Stalport, M. (Creator), Suarez, O. (Creator), Sulis, S. (Creator), GyM., S. (Creator), Udry, S. (Creator), Van Grootel, V. (Creator), Venturini, J. (Creator), Villaver, E. (Creator), Walton, N. A. (Creator) & Wolter, D. (Creator), Centre de Donnees Strasbourg (CDS), 2024
DOI: 10.26093/cds/vizier.36890052
Dataset

Cite this

Borsato, L., Degen, D., Leleu, A., Hooton, M. J., Egger, J. A., Bekkelien, A., Brandeker, A., Cameron, A. C., Günther, M. N., Nascimbeni, V., Persson, C. M., Bonfanti, A., Wilson, T. G., Correia, A. C. M., Zingales, T., Guillot, T., Triaud, A. H. M. J., Piotto, G., Gandolfi, D., ... Wolter, D. (2024). Characterisation of the warm-Jupiter TOI-1130 system with CHEOPS and photo-dynamical approach. Astronomy & Astrophysics, 689, Article A52. https://doi.org/10.1051/0004-6361/202450974

@article{27de9773c8724ff185b88e3896c5b48a,

title = "Characterisation of the warm-Jupiter TOI-1130 system with CHEOPS and photo-dynamical approach",

abstract = "Context. Among the thousands of exoplanets discovered to date, approximately a few hundred gas giants on short-period orbits are classified as {\textquoteleft}lonely{\textquoteright} and only a few are in a multi-planet system with a smaller companion on a close orbit. The processes that formed multi-planet systems hosting gas giants on close orbits are poorly understood, and only a few examples of this kind of system have been observed and well characterised.Aims. Within the contest of a multi-planet system hosting a gas giant on short orbits, we characterise the TOI-1130 system by measuring masses and orbital parameters. This is a two-transiting planet system with a Jupiter-like planet (c) on a 8.35 days orbit and a Neptune-like planet (b) on an inner (4.07 days) orbit. Both planets show strong anti-correlated transit timing variations (TTVs). Furthermore, radial velocity (RV) analysis showed an additional linear trend, a possible hint of a non-transiting candidate planet on a far outer orbit.Methods. Since 2019, extensive transit and radial velocity observations of the TOI-1130 have been acquired using TESS and various ground-based facilities. We present a new photo-dynamical analysis of all available transit and RV data, with the addition of new CHEOPS and ASTEP+ data, which achieve the best precision to date on the planetary radii and masses and on the timings of each transit.Results. We were able to model interior structure of planet b constraining the presence of a gaseous envelope of H/He, while it was not possible to assess the possible water content. Furthermore, we analysed the resonant state of the two transiting planets, and we found that they lie just outside the resonant region. This could be the result of the tidal evolution that the system underwent. We obtained both masses of the planets with a precision of less than 1.5%, and radii with a precision of about 1% and 3% for planet b and c, respectively.",

keywords = "Methods: data analysis, Methods: observational, Techniques: photometric, Telescopes, Planetary systems",

author = "L. Borsato and D. Degen and A. Leleu and Hooton, {M. J.} and Egger, {J. A.} and A. Bekkelien and A. Brandeker and Cameron, {A. Collier} and G{\"u}nther, {M. N.} and V. Nascimbeni and Persson, {C. M.} and A. Bonfanti and Wilson, {T. G.} and Correia, {A. C. M.} and T. Zingales and T. Guillot and Triaud, {A. H. M. J.} and G. Piotto and D. Gandolfi and L. Abe and Y. Alibert and R. Alonso and T. B{\'a}rczy and {Barrado Navascues}, D. and Barros, {S. C. C.} and W. Baumjohann and T. Beck and P. Bendjoya and W. Benz and N. Billot and C. Broeg and Busch, {M. -D.} and Sz Csizmadia and Cubillos, {P. E.} and Davies, {M. B.} and M. Deleuil and A. Deline and L. Delrez 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 L. Fossati and M. Fridlund and K. Gazeas and M. Gillon and M. G{\"u}del and A. Heitzmann and Ch Helling and S. Hoyer 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 D. Magrin and L. Marafatto and Maxted, {P. F. L.} and M. Mecina and D. M{\'e}karnia and C. Mordasini and D. Mura and G. Olofsson and R. Ottensamer and I. Pagano and E. Pall{\'e} and G. Peter and D. Pollacco and D. Queloz and R. Ragazzoni and N. Rando and F. Ratti and H. Rauer and I. Ribas and S. Salmon 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 M. Stalport and O. Suarez and S. Sulis and Szab{\'o}, {Gy M.} and S. Udry and {Van Grootel}, V. and J. Venturini and E. Villaver and Walton, {N. A.} and D. Wolter",

note = "Funding: The Birmingham contribution to ASTEP+ is supported by the European Union{\textquoteright}s Horizon 2020 research and innovation programme (grant{\textquoteright}s agreement no. 803193/BEBOP), and from the Science and Technology Facilities Council (STFC; grant no. ST/S00193X/1, and ST/W002582/1). ABr was supported by the SNSA. ACC acknowledges support from STFC consolidated grant number ST/V000861/1, and UKSA grant number ST/X002217/1. TWi acknowledges support from the UKSA and the University of Warwick. CHe acknowledges support from the European Union H2020-MSCA-ITN-2019 under Grant Agreement no. 860470 (CHAMELEON). P.M. acknowledges support from STFC research grant number ST/R000638/1. NCSa acknowledges funding by the European Union (ERC, FIERCE, 101052347). N.A.W. acknowledges UKSA grant ST/R004838/1. A.H.M.J.T. acknowledges receiving funding from the Science and Technology Facilities Council (STFC; grant n° ST/S00193X/1).",

year = "2024",

month = sep,

doi = "10.1051/0004-6361/202450974",

language = "English",

volume = "689",

journal = "Astronomy & Astrophysics",

issn = "0004-6361",

publisher = "EDP SCIENCES S A",

}

Borsato, L, Degen, D, Leleu, A, Hooton, MJ, Egger, JA, Bekkelien, A, Brandeker, A, Cameron, AC, Günther, MN, Nascimbeni, V, Persson, CM, Bonfanti, A, Wilson, TG, Correia, ACM, Zingales, T, Guillot, T, Triaud, AHMJ, Piotto, G, Gandolfi, D, Abe, L, Alibert, Y, Alonso, R, Bárczy, T, Barrado Navascues, D, Barros, SCC, Baumjohann, W, Beck, T, Bendjoya, P, Benz, W, Billot, N, Broeg, C, Busch, M-D, Csizmadia, S, Cubillos, PE, Davies, MB, Deleuil, M, Deline, A, Delrez, L, Demangeon, ODS, Demory, B-O, Derekas, A, Edwards, B, Ehrenreich, D, Erikson, A, Fortier, A, Fossati, L, Fridlund, M, Gazeas, K, Gillon, M, Güdel, M, Heitzmann, A, Helling, C, Hoyer, S, Isaak, KG, Kiss, LL, Korth, J, Lam, KWF, Laskar, J, Lecavelier des Etangs, A, Lendl, M, Magrin, D, Marafatto, L, Maxted, PFL, Mecina, M, Mékarnia, D, Mordasini, C, Mura, D, Olofsson, G, Ottensamer, R, Pagano, I, Pallé, E, Peter, G, Pollacco, D, Queloz, D, Ragazzoni, R, Rando, N, Ratti, F, Rauer, H, Ribas, I, Salmon, S, Santos, NC, Scandariato, G, Ségransan, D, Simon, AE, Smith, AMS, Sousa, SG, Stalport, M, Suarez, O, Sulis, S, Szabó, GM, Udry, S, Van Grootel, V, Venturini, J, Villaver, E, Walton, NA & Wolter, D 2024, 'Characterisation of the warm-Jupiter TOI-1130 system with CHEOPS and photo-dynamical approach', Astronomy & Astrophysics, vol. 689, A52. https://doi.org/10.1051/0004-6361/202450974

TY - JOUR

T1 - Characterisation of the warm-Jupiter TOI-1130 system with CHEOPS and photo-dynamical approach

AU - Borsato, L.

AU - Degen, D.

AU - Leleu, A.

AU - Hooton, M. J.

AU - Egger, J. A.

AU - Bekkelien, A.

AU - Brandeker, A.

AU - Cameron, A. Collier

AU - Günther, M. N.

AU - Nascimbeni, V.

AU - Persson, C. M.

AU - Bonfanti, A.

AU - Wilson, T. G.

AU - Correia, A. C. M.

AU - Zingales, T.

AU - Guillot, T.

AU - Triaud, A. H. M. J.

AU - Piotto, G.

AU - Gandolfi, D.

AU - Abe, L.

AU - Alibert, Y.

AU - Alonso, R.

AU - Bárczy, T.

AU - Barrado Navascues, D.

AU - Barros, S. C. C.

AU - Baumjohann, W.

AU - Beck, T.

AU - Bendjoya, P.

AU - Benz, W.

AU - Billot, N.

AU - Broeg, C.

AU - Busch, M. -D.

AU - Csizmadia, Sz

AU - Cubillos, P. E.

AU - Davies, M. B.

AU - Deleuil, M.

AU - Deline, A.

AU - Delrez, L.

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 - Fossati, L.

AU - Fridlund, M.

AU - Gazeas, K.

AU - Gillon, M.

AU - Güdel, M.

AU - Heitzmann, A.

AU - Helling, Ch

AU - Hoyer, S.

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 - Magrin, D.

AU - Marafatto, L.

AU - Maxted, P. F. L.

AU - Mecina, M.

AU - Mékarnia, D.

AU - Mordasini, C.

AU - Mura, D.

AU - Olofsson, G.

AU - Ottensamer, R.

AU - Pagano, I.

AU - Pallé, E.

AU - Peter, G.

AU - Pollacco, D.

AU - Queloz, D.

AU - Ragazzoni, R.

AU - Rando, N.

AU - Ratti, F.

AU - Rauer, H.

AU - Ribas, I.

AU - Salmon, S.

AU - Santos, N. C.

AU - Scandariato, G.

AU - Ségransan, D.

AU - Simon, A. E.

AU - Smith, A. M. S.

AU - Sousa, S. G.

AU - Stalport, M.

AU - Suarez, O.

AU - Sulis, S.

AU - Szabó, Gy M.

AU - Udry, S.

AU - Van Grootel, V.

AU - Venturini, J.

AU - Villaver, E.

AU - Walton, N. A.

AU - Wolter, D.

N1 - Funding: The Birmingham contribution to ASTEP+ is supported by the European Union’s Horizon 2020 research and innovation programme (grant’s agreement no. 803193/BEBOP), and from the Science and Technology Facilities Council (STFC; grant no. ST/S00193X/1, and ST/W002582/1). ABr was supported by the SNSA. ACC acknowledges support from STFC consolidated grant number ST/V000861/1, and UKSA grant number ST/X002217/1. TWi acknowledges support from the UKSA and the University of Warwick. CHe acknowledges support from the European Union H2020-MSCA-ITN-2019 under Grant Agreement no. 860470 (CHAMELEON). P.M. acknowledges support from STFC research grant number ST/R000638/1. NCSa acknowledges funding by the European Union (ERC, FIERCE, 101052347). N.A.W. acknowledges UKSA grant ST/R004838/1. A.H.M.J.T. acknowledges receiving funding from the Science and Technology Facilities Council (STFC; grant n° ST/S00193X/1).

PY - 2024/9

Y1 - 2024/9

N2 - Context. Among the thousands of exoplanets discovered to date, approximately a few hundred gas giants on short-period orbits are classified as ‘lonely’ and only a few are in a multi-planet system with a smaller companion on a close orbit. The processes that formed multi-planet systems hosting gas giants on close orbits are poorly understood, and only a few examples of this kind of system have been observed and well characterised.Aims. Within the contest of a multi-planet system hosting a gas giant on short orbits, we characterise the TOI-1130 system by measuring masses and orbital parameters. This is a two-transiting planet system with a Jupiter-like planet (c) on a 8.35 days orbit and a Neptune-like planet (b) on an inner (4.07 days) orbit. Both planets show strong anti-correlated transit timing variations (TTVs). Furthermore, radial velocity (RV) analysis showed an additional linear trend, a possible hint of a non-transiting candidate planet on a far outer orbit.Methods. Since 2019, extensive transit and radial velocity observations of the TOI-1130 have been acquired using TESS and various ground-based facilities. We present a new photo-dynamical analysis of all available transit and RV data, with the addition of new CHEOPS and ASTEP+ data, which achieve the best precision to date on the planetary radii and masses and on the timings of each transit.Results. We were able to model interior structure of planet b constraining the presence of a gaseous envelope of H/He, while it was not possible to assess the possible water content. Furthermore, we analysed the resonant state of the two transiting planets, and we found that they lie just outside the resonant region. This could be the result of the tidal evolution that the system underwent. We obtained both masses of the planets with a precision of less than 1.5%, and radii with a precision of about 1% and 3% for planet b and c, respectively.

AB - Context. Among the thousands of exoplanets discovered to date, approximately a few hundred gas giants on short-period orbits are classified as ‘lonely’ and only a few are in a multi-planet system with a smaller companion on a close orbit. The processes that formed multi-planet systems hosting gas giants on close orbits are poorly understood, and only a few examples of this kind of system have been observed and well characterised.Aims. Within the contest of a multi-planet system hosting a gas giant on short orbits, we characterise the TOI-1130 system by measuring masses and orbital parameters. This is a two-transiting planet system with a Jupiter-like planet (c) on a 8.35 days orbit and a Neptune-like planet (b) on an inner (4.07 days) orbit. Both planets show strong anti-correlated transit timing variations (TTVs). Furthermore, radial velocity (RV) analysis showed an additional linear trend, a possible hint of a non-transiting candidate planet on a far outer orbit.Methods. Since 2019, extensive transit and radial velocity observations of the TOI-1130 have been acquired using TESS and various ground-based facilities. We present a new photo-dynamical analysis of all available transit and RV data, with the addition of new CHEOPS and ASTEP+ data, which achieve the best precision to date on the planetary radii and masses and on the timings of each transit.Results. We were able to model interior structure of planet b constraining the presence of a gaseous envelope of H/He, while it was not possible to assess the possible water content. Furthermore, we analysed the resonant state of the two transiting planets, and we found that they lie just outside the resonant region. This could be the result of the tidal evolution that the system underwent. We obtained both masses of the planets with a precision of less than 1.5%, and radii with a precision of about 1% and 3% for planet b and c, respectively.

KW - Methods: data analysis

KW - Methods: observational

KW - Techniques: photometric

KW - Telescopes

KW - Planetary systems

U2 - 10.1051/0004-6361/202450974

DO - 10.1051/0004-6361/202450974

M3 - Article

SN - 0004-6361

VL - 689

JO - Astronomy & Astrophysics

JF - Astronomy & Astrophysics

M1 - A52

ER -

Characterisation of the warm-Jupiter TOI-1130 system with CHEOPS and photo-dynamical approach

Abstract

Keywords

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Projects

REVEAL: REVEALing Signatures of Habitable Worlds Hidden by Stellar Activity

AO2 - Professor Andrew Cameron: Project AO2 - Andrew Cameron

H2020 MSCA ITN EJD 2019: H2020 MSCA ITN EJD 2019 CHAMELEON

Datasets

TOI-1130 CHEOPS observations

Cite this