November
2023
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2023A&A...679A..33D
Authors
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Damasso, M.
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Rodrigues, J.
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Castro-González, A.
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Lavie, B.
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Davoult, J.
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Zapatero Osorio, M. R.
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Dou, J.
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Sousa, S. G.
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Owen, J. E.
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Sossi, P.
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Adibekyan, V.
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Osborn, H.
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Leinhardt, Z.
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Alibert, Y.
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Lovis, C.
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Delgado Mena, E.
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Sozzetti, A.
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Barros, S. C. C.
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Bossini, D.
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Ziegler, C.
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Ciardi, D. R.
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Matthews, E. C.
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Carter, P. J.
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Lillo-Box, J.
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Suárez Mascareño, A.
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Cristiani, S.
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Pepe, F.
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Rebolo, R.
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Santos, N. C.
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Allende Prieto, C.
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Benatti, S.
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Bouchy, F.
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Briceño, C.
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Di Marcantonio, P.
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D'Odorico, V.
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Dumusque, X.
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Egger, J. A.
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Ehrenreich, D.
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Faria, J.
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Figueira, P.
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Génova Santos, R.
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Gonzales, E. J.
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González Hernández, J. I.
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Law, N.
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Lo Curto, G.
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Mann, A. W.
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Martins, C. J. A. P.
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Mehner, A.
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Micela, G.
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Molaro, P.
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Nunes, N. J.
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Palle, E.
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Poretti, E.
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Schlieder, J. E.
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Udry, S.
Abstract
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Context. One of the goals of the Echelle Spectrograph for Rocky Exoplanets and Stable Spectroscopic Observations (ESPRESSO) Guaranteed Time Observations (GTO) consortium is the precise characterisation of a selected sample of planetary systems discovered by TESS. One such target is the K0V star HIP 29442 (TOI-469), already known to host a validated sub-Neptune companion TOI-469.01, which we followed-up with ESPRESSO.
Aims: We aim to verify the planetary nature of TOI-469.01 by obtaining precise mass, radius, and ephemeris, and constraining its bulk physical structure and composition.
Methods: Following a Bayesian approach, we modelled radial velocity and photometric time series to measure the dynamical mass, radius, and ephemeris, and to characterise the internal structure and composition of TOI-469.01.
Results: We confirmed the planetary nature of TOI-469.01 (now renamed HIP 29442 b), and thanks to the ESPRESSO radial velocities we discovered two additional close-in companions. Through an in-depth analysis of the TESS light curve, we could also detect their low signal-to-noise transit signals. We characterised the additional companions, and conclude that HIP 29442 is a compact multi-planet system. The three planets have orbital periods Porb,b = 13.63083 ± 0.00003, Porb,c = 3.53796 ± 0.00003, and Porb,d = 6.42975−0.00010+0.00009 days, and we measured their masses with high precision: mp,b = 9.6 ± 0.8 M⊕, mp,c = 4.5 ± 0.3 M⊕, and mp,d = 5.1 ± 0.4 M⊕. We measured radii and bulk densities of all the planets (the 3σ confidence intervals are shown in parentheses): Rp,b = 3.48−0.08(−0.28)+0.07(+0.19) R⊕ and ρp,b = 1.3 ± 0.2(0.3)g cm−3; Rp,c = 1.58−0.11(−0.34)+0.10(+0.30) R⊕ and ρp,c = 6.3−1.3(−2.7)+1.7(+6.0)g cm−3; Rp,d = 1.37 ± 0.11(−0.43)(+0.32) R⊕ and ρp,d = 11.0−2.4(−6.3)+3.4(+21.0)g cm−3. Due to noisy light curves, we used the more conservative 3σ confidence intervals for the radii as input to the interior structure modelling. We find that HIP 29442 b appears as a typical sub-Neptune, likely surrounded by a gas layer of pure H-He with amass of 0.27−0.17+0.24 M⊕ and a thickness of 1.4 ± 0.5 R⊕. For the innermost companions HIP 29442 c and HIP 29442 d, the model supports an Earth-like composition.
Conclusions: The compact multi-planet system orbiting HIP 29442 offers the opportunity to study simultaneously planets straddling the gap in the observed radius distribution of close-in small-size exoplanets. High-precision photometric follow-up is required to obtain more accurate and precise radius measurements, especially for planets c and d. This, together with our determined high-precision masses, will provide the accurate and precise bulk structure of the planets, and enable an accurate investigation of the system's evolution.
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