Unveiling the internal structure and formation history of the three planets transiting HIP 29442 (TOI-469) with CHEOPS

J. A. Egger; H. P. Osborn; D. Kubyshkina; C. Mordasini; Y. Alibert; M. N. Günther; M. Lendl; A. Brandeker; A. Heitzmann; A. Leleu; M. Damasso; A. Bonfanti; T. G. Wilson; S. G. Sousa; J. Haldemann; L. Delrez; M. J. Hooton; T. Zingales; R. Luque; R. Alonso; J. Asquier; T. Bárczy; D.  Barrado Navascues; S. C. C. Barros; W. Baumjohann; W. Benz; N. Billot; L. Borsato; C. Broeg; M. Buder; A. Castro-González; A. Collier Cameron; A. C. M. Correia; D. Cortes; 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; L. Fossati; M. Fridlund; D. Gandolfi; K. Gazeas; M. Gillon; M. Güdel; Ch Helling; K. G. Isaak; L. L. Kiss; J. Korth; K. W. F. Lam; J. Laskar; B. Lavie; A. Lecavelier des Etangs; C. Lovis; A. Luntzer; D. Magrin; P. F. L. Maxted; B. Merín; M. Munari; V. Nascimbeni; G. Olofsson; R. Ottensamer; I. Pagano; E. Pallé; G. Peter; D. Piazza; G. Piotto; D. Pollacco; D. Queloz; R. Ragazzoni; N. Rando; H. Rauer; I. Ribas; J. Rodrigues; N. C. Santos; G. Scandariato; D. Ségransan; A. E. Simon; A. M. S. Smith; M. Stalport; S. Sulis; Gy M. Szabó; S. Udry; V. Van Grootel; J. Venturini; E. Villaver; N. A. Walton

doi:10.1051/0004-6361/202450472

Unveiling the internal structure and formation history of the three planets transiting HIP 29442 (TOI-469) with CHEOPS

J. A. Egger^*, H. P. Osborn, D. Kubyshkina, C. Mordasini, Y. Alibert, M. N. Günther, M. Lendl, A. Brandeker, A. Heitzmann, A. Leleu, M. Damasso, A. Bonfanti, T. G. Wilson, S. G. Sousa, J. Haldemann, L. Delrez, M. J. Hooton, T. Zingales, R. Luque, R. AlonsoJ. Asquier, T. Bárczy, D. Barrado Navascues, S. C. C. Barros, W. Baumjohann, W. Benz, N. Billot, L. Borsato, C. Broeg, M. Buder, A. Castro-González, A. Collier Cameron, A. C. M. Correia, D. Cortes, 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, L. Fossati, M. Fridlund, D. Gandolfi, K. Gazeas, M. Gillon, M. Güdel, Ch Helling, K. G. Isaak, L. L. Kiss, J. Korth, K. W. F. Lam, J. Laskar, B. Lavie, A. Lecavelier des Etangs, C. Lovis, A. Luntzer, D. Magrin, P. F. L. Maxted, B. Merín, M. Munari, V. Nascimbeni, G. Olofsson, R. Ottensamer, I. Pagano, E. Pallé, G. Peter, D. Piazza, G. Piotto, D. Pollacco, D. Queloz, R. Ragazzoni, N. Rando, H. Rauer, I. Ribas, J. Rodrigues, N. C. Santos, G. Scandariato, D. Ségransan, A. E. Simon, A. M. S. Smith, M. Stalport, S. Sulis, Gy M. Szabó, S. Udry, V. Van Grootel, J. Venturini, E. Villaver, N. A. Walton

^*Corresponding author for this work

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

Abstract

Multiplanetary systems spanning the radius valley are ideal testing grounds for exploring the different proposed explanations for the observed bimodality in the radius distribution of close-in exoplanets. One such system is HIP 29442 (TOI-469), an evolved K0V star hosting two super-Earths and one sub-Neptune. We observed HIP 29442 with CHEOPS for a total of 9.6 days, which we modelled jointly with two sectors of TESS data to derive planetary radii of 3.410 ± 0.046, 1.551 ± 0.045, and 1.538 ± 0.049 R⊕ for planets b, c, and d, which orbit HIP 29442 with periods of 13.6, 3.5, and 6.4 days, respectively. For planet d this value deviates by more than 3σ from the median value reported in the discovery paper, leading us to conclude that caution is required when using TESS photometry to determine the radii of small planets with low per-transit signal-to-noise ratios and large gaps between observations. Given the high precision of these new radii, combining them with published RVs from ESPRESSO and HIRES provides us with ideal conditions to investigate the internal structure and formation pathways of the planets in the system. We introduced the publicly available code plaNETic, a fast and robust neural network-based Bayesian internal structure modelling framework. We then applied hydrodynamic models to explore the upper atmospheric properties of these inferred structures. Finally, we identified planetary system analogues in a synthetic population generated with the Bern model for planet formation and evolution. Based on this analysis, we find that the planets likely formed on opposing sides of the water iceline from a protoplanetary disk with an intermediate solid mass. We finally report that the observed parameters of the HIP 29442 system are compatible with a scenario where the second peak in the bimodal radius distribution corresponds to sub-Neptunes with a pure H/He envelope and with a scenario with water-rich sub-Neptunes.

Original language	English
Article number	A223
Number of pages	30
Journal	Astronomy & Astrophysics
Volume	688
Early online date	27 Aug 2024
DOIs	https://doi.org/10.1051/0004-6361/202450472
Publication status	Published - Aug 2024

Keywords

Techniques: photometric
Planets and satellites: formation
Planets and satellites: interiors
Planets and satellites: individual: HIP 29442
Planetary systems

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https://arxiv.org/abs/2406.18653Licence: Other

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REVEAL: REVEALing Signatures of Habitable Worlds Hidden by Stellar Activity
Cameron, A. C. (PI)
UKRI (EU)
1/08/24 → 31/07/30
Project: Standard
AO2 - Professor Andrew Cameron: Project AO2 - Andrew Cameron
Cameron, A. C. (PI)
Science & Technology Facilities Council
1/04/21 → 31/03/24
Project: Standard

HIP 29442 (TOI-469) CHEOPS and TESS light curves
Egger, J. A. (Creator), Osborn, H. P. (Creator), Kubyshkina, D. (Creator), Mordasini, C. (Creator), Alibert, Y. (Creator), Guenther, M. N. (Creator), Lendl, M. (Creator), Brandeker, A. (Creator), Heitzmann, A. (Creator), Leleu, A. (Creator), Damasso, M. (Creator), Bonfanti, A. (Creator), Wilson, T. G. (Creator), Sousa, S. G. (Creator), Haldemann, J. (Creator), Delrez, L. (Creator), Hooton, M. J. (Creator), Zingales, T. (Creator), Luque, R. (Creator), Alonso, R. (Creator), Asquier, J. (Creator), Barczy, T. (Creator), Barrado Navascues, D. (Creator), Barros, S. C. C. (Creator), Baumjohann, W. (Creator), Benz, W. (Creator), Billot, N. (Creator), Borsato, L. (Creator), Broeg, C. (Creator), Buder, M. (Creator), Castro-Gonzalez, A. (Creator), Collier Cameron, A. (Creator), Correia, A. C. M. (Creator), Cortes, D. (Creator), Sz, C. (Creator), Cubillos, P. E. (Creator), Davies, M. B. (Creator), Deleuil, M. (Creator), Deline, A. (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), Gandolfi, D. (Creator), Gazeas, K. (Creator), Gillon, M. (Creator), Guedel, M. (Creator), Ch, H. (Creator), Isaak, K. G. (Creator), Kiss, L. L. (Creator), Korth, J. (Creator), K.W.F., L. (Creator), Laskar, J. (Creator), Lavie, B. (Creator), Lecavelier Des Etangs, A. (Creator), Lovis, C. (Creator), Luntzer, A. (Creator), Magrin, D. (Creator), Maxted, P. F. L. (Creator), Merin, B. (Creator), Munari, M. (Creator), Nascimbeni, V. (Creator), Olofsson, G. (Creator), Ottensamer, R. (Creator), Pagano, I. (Creator), Palle, E. (Creator), Peter, G. (Creator), Piazza, D. (Creator), Piotto, G. (Creator), Pollacco, D. (Creator), Queloz, D. (Creator), Ragazzoni, R. (Creator), Rando, N. (Creator), Rauer, H. (Creator), Ribas, I. (Creator), Rodrigues, J. (Creator), Santos, N. C. (Creator), Scandariato, G. (Creator), Segransan, D. (Creator), Simon, A. E. (Creator), Smith, A. M. S. (Creator), Stalport, M. (Creator), Sulis, S. (Creator), GyM., S. (Creator), Udry, S. (Creator), Van Grootel, V. (Creator), Venturini, J. (Creator), Villaver, E. (Creator) & Walton, N. A. (Creator), Centre de Donnees Strasbourg (CDS), 2024
DOI: 10.26093/cds/vizier.36880223
Dataset

Cite this

Egger, J. A., Osborn, H. P., Kubyshkina, D., Mordasini, C., Alibert, Y., Günther, M. N., Lendl, M., Brandeker, A., Heitzmann, A., Leleu, A., Damasso, M., Bonfanti, A., Wilson, T. G., Sousa, S. G., Haldemann, J., Delrez, L., Hooton, M. J., Zingales, T., Luque, R., ... Walton, N. A. (2024). Unveiling the internal structure and formation history of the three planets transiting HIP 29442 (TOI-469) with CHEOPS. Astronomy & Astrophysics, 688, Article A223. https://doi.org/10.1051/0004-6361/202450472

@article{dc4c5d08eca2416f9ebd76b85fa4c084,

title = "Unveiling the internal structure and formation history of the three planets transiting HIP 29442 (TOI-469) with CHEOPS",

abstract = "Multiplanetary systems spanning the radius valley are ideal testing grounds for exploring the different proposed explanations for the observed bimodality in the radius distribution of close-in exoplanets. One such system is HIP 29442 (TOI-469), an evolved K0V star hosting two super-Earths and one sub-Neptune. We observed HIP 29442 with CHEOPS for a total of 9.6 days, which we modelled jointly with two sectors of TESS data to derive planetary radii of 3.410 ± 0.046, 1.551 ± 0.045, and 1.538 ± 0.049 R⊕ for planets b, c, and d, which orbit HIP 29442 with periods of 13.6, 3.5, and 6.4 days, respectively. For planet d this value deviates by more than 3σ from the median value reported in the discovery paper, leading us to conclude that caution is required when using TESS photometry to determine the radii of small planets with low per-transit signal-to-noise ratios and large gaps between observations. Given the high precision of these new radii, combining them with published RVs from ESPRESSO and HIRES provides us with ideal conditions to investigate the internal structure and formation pathways of the planets in the system. We introduced the publicly available code plaNETic, a fast and robust neural network-based Bayesian internal structure modelling framework. We then applied hydrodynamic models to explore the upper atmospheric properties of these inferred structures. Finally, we identified planetary system analogues in a synthetic population generated with the Bern model for planet formation and evolution. Based on this analysis, we find that the planets likely formed on opposing sides of the water iceline from a protoplanetary disk with an intermediate solid mass. We finally report that the observed parameters of the HIP 29442 system are compatible with a scenario where the second peak in the bimodal radius distribution corresponds to sub-Neptunes with a pure H/He envelope and with a scenario with water-rich sub-Neptunes.",

keywords = "Techniques: photometric, Planets and satellites: formation, Planets and satellites: interiors, Planets and satellites: individual: HIP 29442, Planetary systems",

author = "Egger, {J. A.} and Osborn, {H. P.} and D. Kubyshkina and C. Mordasini and Y. Alibert and G{\"u}nther, {M. N.} and M. Lendl and A. Brandeker and A. Heitzmann and A. Leleu and M. Damasso and A. Bonfanti and Wilson, {T. G.} and Sousa, {S. G.} and J. Haldemann and L. Delrez and Hooton, {M. J.} and T. Zingales and R. Luque and R. Alonso and J. Asquier and T. B{\'a}rczy and {Barrado Navascues}, D. and Barros, {S. C. C.} and W. Baumjohann and W. Benz and N. Billot and L. Borsato and C. Broeg and M. Buder and A. Castro-Gonz{\'a}lez and Cameron, {A. Collier} and Correia, {A. C. M.} and D. Cortes 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 L. Fossati and M. Fridlund and D. Gandolfi and K. Gazeas and M. Gillon and M. G{\"u}del and Ch Helling and Isaak, {K. G.} and Kiss, {L. L.} and J. Korth and Lam, {K. W. F.} and J. Laskar and B. Lavie and {Lecavelier des Etangs}, A. and C. Lovis and A. Luntzer and D. Magrin and Maxted, {P. F. L.} and B. Mer{\'i}n 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 D. Queloz and R. Ragazzoni and N. Rando and H. Rauer and I. Ribas and J. Rodrigues and Santos, {N. C.} and G. Scandariato and D. S{\'e}gransan and Simon, {A. E.} and Smith, {A. M. S.} and M. Stalport 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.}",

note = "Funding: A.C.C. acknowledges support from STFC consolidated grant numbers ST/R000824/1 and ST/V000861/1, and UKSA grant number ST/R003203/1. CHe acknowledges support from the European Union H2020-MSCA-ITN-2019 under Grant Agreement no. 860470 (CHAMELEON). PM acknowledges support from STFC research grant number ST/R000638/1. NCSa acknowledges funding by the European Union (ERC, FIERCE, 101052347). NAW acknowledges UKSA grant ST/R004838/1.",

year = "2024",

month = aug,

doi = "10.1051/0004-6361/202450472",

language = "English",

volume = "688",

journal = "Astronomy & Astrophysics",

issn = "0004-6361",

publisher = "EDP SCIENCES S A",

}

Egger, JA, Osborn, HP, Kubyshkina, D, Mordasini, C, Alibert, Y, Günther, MN, Lendl, M, Brandeker, A, Heitzmann, A, Leleu, A, Damasso, M, Bonfanti, A, Wilson, TG, Sousa, SG, Haldemann, J, Delrez, L, Hooton, MJ, Zingales, T, Luque, R, Alonso, R, Asquier, J, Bárczy, T, Barrado Navascues, D, Barros, SCC, Baumjohann, W, Benz, W, Billot, N, Borsato, L, Broeg, C, Buder, M, Castro-González, A, Cameron, AC, Correia, ACM, Cortes, D, Csizmadia, S, Cubillos, PE, Davies, MB, Deleuil, M, Deline, A, Demangeon, ODS, Demory, B-O, Derekas, A, Edwards, B, Ehrenreich, D, Erikson, A, Fortier, A, Fossati, L, Fridlund, M, Gandolfi, D, Gazeas, K, Gillon, M, Güdel, M, Helling, C, Isaak, KG, Kiss, LL, Korth, J, Lam, KWF, Laskar, J, Lavie, B, Lecavelier des Etangs, A, Lovis, C, Luntzer, A, Magrin, D, Maxted, PFL, Merín, B, Munari, M, Nascimbeni, V, Olofsson, G, Ottensamer, R, Pagano, I, Pallé, E, Peter, G, Piazza, D, Piotto, G, Pollacco, D, Queloz, D, Ragazzoni, R, Rando, N, Rauer, H, Ribas, I, Rodrigues, J, Santos, NC, Scandariato, G, Ségransan, D, Simon, AE, Smith, AMS, Stalport, M, Sulis, S, Szabó, GM, Udry, S, Van Grootel, V, Venturini, J, Villaver, E & Walton, NA 2024, 'Unveiling the internal structure and formation history of the three planets transiting HIP 29442 (TOI-469) with CHEOPS', Astronomy & Astrophysics, vol. 688, A223. https://doi.org/10.1051/0004-6361/202450472

TY - JOUR

T1 - Unveiling the internal structure and formation history of the three planets transiting HIP 29442 (TOI-469) with CHEOPS

AU - Egger, J. A.

AU - Osborn, H. P.

AU - Kubyshkina, D.

AU - Mordasini, C.

AU - Alibert, Y.

AU - Günther, M. N.

AU - Lendl, M.

AU - Brandeker, A.

AU - Heitzmann, A.

AU - Leleu, A.

AU - Damasso, M.

AU - Bonfanti, A.

AU - Wilson, T. G.

AU - Sousa, S. G.

AU - Haldemann, J.

AU - Delrez, L.

AU - Hooton, M. J.

AU - Zingales, T.

AU - Luque, R.

AU - Alonso, R.

AU - Asquier, J.

AU - Bárczy, T.

AU - Barrado Navascues, D.

AU - Barros, S. C. C.

AU - Baumjohann, W.

AU - Benz, W.

AU - Billot, N.

AU - Borsato, L.

AU - Broeg, C.

AU - Buder, M.

AU - Castro-González, A.

AU - Cameron, A. Collier

AU - Correia, A. C. M.

AU - Cortes, D.

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 - Fossati, L.

AU - Fridlund, M.

AU - Gandolfi, D.

AU - Gazeas, K.

AU - Gillon, M.

AU - Güdel, M.

AU - Helling, Ch

AU - Isaak, K. G.

AU - Kiss, L. L.

AU - Korth, J.

AU - Lam, K. W. F.

AU - Laskar, J.

AU - Lavie, B.

AU - Lecavelier des Etangs, A.

AU - Lovis, C.

AU - Luntzer, A.

AU - Magrin, D.

AU - Maxted, P. F. L.

AU - Merín, B.

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 - Queloz, D.

AU - Ragazzoni, R.

AU - Rando, N.

AU - Rauer, H.

AU - Ribas, I.

AU - Rodrigues, J.

AU - Santos, N. C.

AU - Scandariato, G.

AU - Ségransan, D.

AU - Simon, A. E.

AU - Smith, A. M. S.

AU - Stalport, M.

AU - Sulis, S.

AU - Szabó, Gy M.

AU - Udry, S.

AU - Van Grootel, V.

AU - Venturini, J.

AU - Villaver, E.

AU - Walton, N. A.

N1 - Funding: A.C.C. acknowledges support from STFC consolidated grant numbers ST/R000824/1 and ST/V000861/1, and UKSA grant number ST/R003203/1. CHe acknowledges support from the European Union H2020-MSCA-ITN-2019 under Grant Agreement no. 860470 (CHAMELEON). PM acknowledges support from STFC research grant number ST/R000638/1. NCSa acknowledges funding by the European Union (ERC, FIERCE, 101052347). NAW acknowledges UKSA grant ST/R004838/1.

PY - 2024/8

Y1 - 2024/8

N2 - Multiplanetary systems spanning the radius valley are ideal testing grounds for exploring the different proposed explanations for the observed bimodality in the radius distribution of close-in exoplanets. One such system is HIP 29442 (TOI-469), an evolved K0V star hosting two super-Earths and one sub-Neptune. We observed HIP 29442 with CHEOPS for a total of 9.6 days, which we modelled jointly with two sectors of TESS data to derive planetary radii of 3.410 ± 0.046, 1.551 ± 0.045, and 1.538 ± 0.049 R⊕ for planets b, c, and d, which orbit HIP 29442 with periods of 13.6, 3.5, and 6.4 days, respectively. For planet d this value deviates by more than 3σ from the median value reported in the discovery paper, leading us to conclude that caution is required when using TESS photometry to determine the radii of small planets with low per-transit signal-to-noise ratios and large gaps between observations. Given the high precision of these new radii, combining them with published RVs from ESPRESSO and HIRES provides us with ideal conditions to investigate the internal structure and formation pathways of the planets in the system. We introduced the publicly available code plaNETic, a fast and robust neural network-based Bayesian internal structure modelling framework. We then applied hydrodynamic models to explore the upper atmospheric properties of these inferred structures. Finally, we identified planetary system analogues in a synthetic population generated with the Bern model for planet formation and evolution. Based on this analysis, we find that the planets likely formed on opposing sides of the water iceline from a protoplanetary disk with an intermediate solid mass. We finally report that the observed parameters of the HIP 29442 system are compatible with a scenario where the second peak in the bimodal radius distribution corresponds to sub-Neptunes with a pure H/He envelope and with a scenario with water-rich sub-Neptunes.

AB - Multiplanetary systems spanning the radius valley are ideal testing grounds for exploring the different proposed explanations for the observed bimodality in the radius distribution of close-in exoplanets. One such system is HIP 29442 (TOI-469), an evolved K0V star hosting two super-Earths and one sub-Neptune. We observed HIP 29442 with CHEOPS for a total of 9.6 days, which we modelled jointly with two sectors of TESS data to derive planetary radii of 3.410 ± 0.046, 1.551 ± 0.045, and 1.538 ± 0.049 R⊕ for planets b, c, and d, which orbit HIP 29442 with periods of 13.6, 3.5, and 6.4 days, respectively. For planet d this value deviates by more than 3σ from the median value reported in the discovery paper, leading us to conclude that caution is required when using TESS photometry to determine the radii of small planets with low per-transit signal-to-noise ratios and large gaps between observations. Given the high precision of these new radii, combining them with published RVs from ESPRESSO and HIRES provides us with ideal conditions to investigate the internal structure and formation pathways of the planets in the system. We introduced the publicly available code plaNETic, a fast and robust neural network-based Bayesian internal structure modelling framework. We then applied hydrodynamic models to explore the upper atmospheric properties of these inferred structures. Finally, we identified planetary system analogues in a synthetic population generated with the Bern model for planet formation and evolution. Based on this analysis, we find that the planets likely formed on opposing sides of the water iceline from a protoplanetary disk with an intermediate solid mass. We finally report that the observed parameters of the HIP 29442 system are compatible with a scenario where the second peak in the bimodal radius distribution corresponds to sub-Neptunes with a pure H/He envelope and with a scenario with water-rich sub-Neptunes.

KW - Techniques: photometric

KW - Planets and satellites: formation

KW - Planets and satellites: interiors

KW - Planets and satellites: individual: HIP 29442

KW - Planetary systems

U2 - 10.1051/0004-6361/202450472

DO - 10.1051/0004-6361/202450472

M3 - Article

SN - 0004-6361

VL - 688

JO - Astronomy & Astrophysics

JF - Astronomy & Astrophysics

M1 - A223

ER -

Unveiling the internal structure and formation history of the three planets transiting HIP 29442 (TOI-469) with CHEOPS

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Keywords

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REVEAL: REVEALing Signatures of Habitable Worlds Hidden by Stellar Activity

AO2 - Professor Andrew Cameron: Project AO2 - Andrew Cameron

Datasets

HIP 29442 (TOI-469) CHEOPS and TESS light curves

Cite this