A new dynamical modeling of the WASP-47 system with CHEOPS observations

V. Nascimbeni; L. Borsato; T. Zingales; G. Piotto; I. Pagano; M. Beck; C. Broeg; D. Ehrenreich; S. Hoyer; F.~Z. Majidi; V. Granata; S.~G. Sousa; T.~G. Wilson; V. Van Grootel; A. Bonfanti; S. Salmon; A.~J. Mustill; L. Delrez; Y. Alibert; R. Alonso; G. Anglada; T. Bárczy; D. Barrado; S.~C.~C. Barros; W. Baumjohann; T. Beck; W. Benz; M. Bergomi; N. Billot; X. Bonfils; A. Brandeker; J. Cabrera; S. Charnoz; A. Collier Cameron; Sz. Csizmadia; P.~E. Cubillos; M.~B. Davies; M. Deleuil; A. Deline; O.~D.~S. Demangeon; B. -O. Demory; A. Erikson; A. Fortier; L. Fossati; M. Fridlund; D. Gandolfi; M. Gillon; M. Güdel; K.~G. Isaak; L.~L. Kiss; J. Laskar; A. Lecavelier des Etangs; M. Lendl; C. Lovis; R. Luque; D. Magrin; P.~F.~L. Maxted; C. Mordasini; G. Olofsson; R. Ottensamer; E. Pallé; G. Peter; D. Piazza; D. Pollacco; D. Queloz; R. Ragazzoni; N. Rando; F. Ratti; H. Rauer; I. Ribas; N.~C. Santos; G. Scandariato; D. Ségransan; A.~E. Simon; A.~M.~S. Smith; M. Steinberger; M. Steller; Gy. M. Szabó; N. Thomas; S. Udry; J. Venturini; N.~A. Walton; D. Wolter

doi:10.1051/0004-6361/202245486

A new dynamical modeling of the WASP-47 system with CHEOPS observations

V. Nascimbeni, L. Borsato, T. Zingales, G. Piotto, I. Pagano, M. Beck, C. Broeg, D. Ehrenreich, S. Hoyer, F.~Z. Majidi, V. Granata, S.~G. Sousa, T.~G. Wilson, V. Van Grootel, A. Bonfanti, S. Salmon, A.~J. Mustill, L. Delrez, Y. Alibert, R. AlonsoG. Anglada, T. Bárczy, D. Barrado, S.~C.~C. Barros, W. Baumjohann, T. Beck, W. Benz, M. Bergomi, N. Billot, X. Bonfils, A. Brandeker, J. Cabrera, S. Charnoz, A. Collier Cameron, Sz. Csizmadia, P.~E. Cubillos, M.~B. Davies, M. Deleuil, A. Deline, O.~D.~S. Demangeon, B. -O. Demory, A. Erikson, A. Fortier, L. Fossati, M. Fridlund, D. Gandolfi, M. Gillon, M. Güdel, K.~G. Isaak, L.~L. Kiss, J. Laskar, A. Lecavelier des Etangs, M. Lendl, C. Lovis, R. Luque, D. Magrin, P.~F.~L. Maxted, C. Mordasini, G. Olofsson, R. Ottensamer, E. Pallé, G. Peter, D. Piazza, D. Pollacco, D. Queloz, R. Ragazzoni, N. Rando, F. Ratti, H. Rauer, I. Ribas, N.~C. Santos, G. Scandariato, D. Ségransan, A.~E. Simon, A.~M.~S. Smith, M. Steinberger, M. Steller, Gy. M. Szabó, N. Thomas, S. Udry, J. Venturini, N.~A. Walton, D. Wolter

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

Abstract

Among the hundreds of known hot Jupiters (HJs), only five have been found to have companions on short-period orbits. Within this rare class of multiple planetary systems, the architecture of WASP-47 is unique, hosting an HJ (planet-b) with both an inner and an outer sub-Neptunian mass companion (-e and -d, respectively) as well as an additional non-transiting, long-period giant (-c). The small period ratio between planets -b and -d boosts the transit time variation (TTV) signal, making it possible to reliably measure the masses of these planets in synergy with the radial velocity (RV) technique. In this paper, we present new space- and ground-based photometric data of WASP-47b and WASP-47-d, including 11 unpublished light curves from the ESA mission CHaracterising ExOPlanet Satellite (CHEOPS). We analyzed the light curves in a homogeneous way together with all the publicly available data to carry out a global N-body dynamical modeling of the TTV and RV signals. We retrieved, among other parameters, a mass and density for planet -d of Md = 15.5 ± 0.8 M⊕ and ρd = 1.69 ± 0.22 g cm−3, which is in good agreement with the literature and consistent with a Neptune-like composition. For the inner planet (-e), we found a mass and density of Me = 9.0 ± 0.5 M⊕ and ρe = 8.1 ± 0.5 g cm−3, suggesting an Earth-like composition close to other ultra-hot planets at similar irradiation levels. Though this result is in agreement with previous RV plus TTV studies, it is not in agreement with the most recent RV analysis (at 2.8σ), which yielded a lower density compatible with a pure silicate composition. This discrepancy highlights the still unresolved issue of suspected systematic offsets between RV and TTV measurements. In this paper, we also significantly improve the orbital ephemerides of all transiting planets, which will be crucial for any future follow-up.

Original language	English
Article number	A42
Journal	Astronomy & Astrophysics
Volume	673
DOIs	https://doi.org/10.1051/0004-6361/202245486
Publication status	Published - 2023 May 1

Subject classification (UKÄ)

Astronomy, Astrophysics and Cosmology

Free keywords

techniques: photometric
planets and satellites: detection
planets and satellites: general
Astrophysics - Earth and Planetary Astrophysics
Astrophysics - Solar and Stellar Astrophysics

Access to Document

10.1051/0004-6361/202245486

Consolidating CHEOPS and preparing for PLATO: Exoplanet studies in the 2020s
Mustill, A. (Researcher)
Swedish National Space Agency
Project: Research

Cite this

Nascimbeni, V., Borsato, L., Zingales, T., Piotto, G., Pagano, I., Beck, M., Broeg, C., Ehrenreich, D., Hoyer, S., Majidi, F. Z., Granata, V., Sousa, S. G., Wilson, T. G., Van Grootel, V., Bonfanti, A., Salmon, S., Mustill, A. J., Delrez, L., Alibert, Y., ... Wolter, D. (2023). A new dynamical modeling of the WASP-47 system with CHEOPS observations. Astronomy & Astrophysics, 673, Article A42. https://doi.org/10.1051/0004-6361/202245486

@article{cb3f8ee19cf94eaa8f97563613da6395,

title = "A new dynamical modeling of the WASP-47 system with CHEOPS observations",

abstract = "Among the hundreds of known hot Jupiters (HJs), only five have been found to have companions on short-period orbits. Within this rare class of multiple planetary systems, the architecture of WASP-47 is unique, hosting an HJ (planet-b) with both an inner and an outer sub-Neptunian mass companion (-e and -d, respectively) as well as an additional non-transiting, long-period giant (-c). The small period ratio between planets -b and -d boosts the transit time variation (TTV) signal, making it possible to reliably measure the masses of these planets in synergy with the radial velocity (RV) technique. In this paper, we present new space- and ground-based photometric data of WASP-47b and WASP-47-d, including 11 unpublished light curves from the ESA mission CHaracterising ExOPlanet Satellite (CHEOPS). We analyzed the light curves in a homogeneous way together with all the publicly available data to carry out a global N-body dynamical modeling of the TTV and RV signals. We retrieved, among other parameters, a mass and density for planet -d of Md = 15.5 ± 0.8 M⊕ and ρd = 1.69 ± 0.22 g cm−3, which is in good agreement with the literature and consistent with a Neptune-like composition. For the inner planet (-e), we found a mass and density of Me = 9.0 ± 0.5 M⊕ and ρe = 8.1 ± 0.5 g cm−3, suggesting an Earth-like composition close to other ultra-hot planets at similar irradiation levels. Though this result is in agreement with previous RV plus TTV studies, it is not in agreement with the most recent RV analysis (at 2.8σ), which yielded a lower density compatible with a pure silicate composition. This discrepancy highlights the still unresolved issue of suspected systematic offsets between RV and TTV measurements. In this paper, we also significantly improve the orbital ephemerides of all transiting planets, which will be crucial for any future follow-up.",

keywords = "techniques: photometric, planets and satellites: detection, planets and satellites: general, Astrophysics - Earth and Planetary Astrophysics, Astrophysics - Solar and Stellar Astrophysics",

author = "V. Nascimbeni and L. Borsato and T. Zingales and G. Piotto and I. Pagano and M. Beck and C. Broeg and D. Ehrenreich and S. Hoyer and F.~Z. Majidi and V. Granata and S.~G. Sousa and T.~G. Wilson and {Van Grootel}, V. and A. Bonfanti and S. Salmon and A.~J. Mustill and L. Delrez and Y. Alibert and R. Alonso and G. Anglada and T. B{\'a}rczy and D. Barrado and S.~C.~C. Barros and W. Baumjohann and T. Beck and W. Benz and M. Bergomi and N. Billot and X. Bonfils and A. Brandeker and J. Cabrera and S. Charnoz and {Collier Cameron}, A. and Sz. Csizmadia and P.~E. Cubillos and M.~B. Davies and M. Deleuil and A. Deline and O.~D.~S. Demangeon and Demory, {B. -O.} and A. Erikson and A. Fortier and L. Fossati and M. Fridlund and D. Gandolfi and M. Gillon and M. G{\"u}del and K.~G. Isaak and L.~L. Kiss and J. Laskar and {Lecavelier des Etangs}, A. and M. Lendl and C. Lovis and R. Luque and D. Magrin and P.~F.~L. Maxted and C. Mordasini and G. Olofsson and R. Ottensamer and E. Pall{\'e} and G. Peter and D. Piazza and D. Pollacco and D. Queloz and R. Ragazzoni and N. Rando and F. Ratti and H. Rauer and I. Ribas and N.~C. Santos and G. Scandariato and D. S{\'e}gransan and A.~E. Simon and A.~M.~S. Smith and M. Steinberger and M. Steller and Szab{\'o}, {Gy. M.} and N. Thomas and S. Udry and J. Venturini and N.~A. Walton and D. Wolter",

year = "2023",

month = may,

day = "1",

doi = "10.1051/0004-6361/202245486",

language = "English",

volume = "673",

journal = "Astronomy & Astrophysics",

issn = "1432-0746",

publisher = "EDP Sciences",

}

Nascimbeni, V, Borsato, L, Zingales, T, Piotto, G, Pagano, I, Beck, M, Broeg, C, Ehrenreich, D, Hoyer, S, Majidi, FZ, Granata, V, Sousa, SG, Wilson, TG, Van Grootel, V, Bonfanti, A, Salmon, S, Mustill, AJ, Delrez, L, Alibert, Y, Alonso, R, Anglada, G, Bárczy, T, Barrado, D, Barros, SCC, Baumjohann, W, Beck, T, Benz, W, Bergomi, M, Billot, N, Bonfils, X, Brandeker, A, Cabrera, J, Charnoz, S, Collier Cameron, A, Csizmadia, S, Cubillos, PE, Davies, MB, Deleuil, M, Deline, A, Demangeon, ODS, Demory, B-O, Erikson, A, Fortier, A, Fossati, L, Fridlund, M, Gandolfi, D, Gillon, M, Güdel, M, Isaak, KG, Kiss, LL, Laskar, J, Lecavelier des Etangs, A, Lendl, M, Lovis, C, Luque, R, Magrin, D, Maxted, PFL, Mordasini, C, Olofsson, G, Ottensamer, R, Pallé, E, Peter, G, Piazza, D, Pollacco, D, Queloz, D, Ragazzoni, R, Rando, N, Ratti, F, Rauer, H, Ribas, I, Santos, NC, Scandariato, G, Ségransan, D, Simon, AE, Smith, AMS, Steinberger, M, Steller, M, Szabó, GM, Thomas, N, Udry, S, Venturini, J, Walton, NA & Wolter, D 2023, 'A new dynamical modeling of the WASP-47 system with CHEOPS observations', Astronomy & Astrophysics, vol. 673, A42. https://doi.org/10.1051/0004-6361/202245486

TY - JOUR

T1 - A new dynamical modeling of the WASP-47 system with CHEOPS observations

AU - Nascimbeni, V.

AU - Borsato, L.

AU - Zingales, T.

AU - Piotto, G.

AU - Pagano, I.

AU - Beck, M.

AU - Broeg, C.

AU - Ehrenreich, D.

AU - Hoyer, S.

AU - Majidi, F.~Z.

AU - Granata, V.

AU - Sousa, S.~G.

AU - Wilson, T.~G.

AU - Van Grootel, V.

AU - Bonfanti, A.

AU - Salmon, S.

AU - Mustill, A.~J.

AU - Delrez, L.

AU - Alibert, Y.

AU - Alonso, R.

AU - Anglada, G.

AU - Bárczy, T.

AU - Barrado, D.

AU - Barros, S.~C.~C.

AU - Baumjohann, W.

AU - Beck, T.

AU - Benz, W.

AU - Bergomi, M.

AU - Billot, N.

AU - Bonfils, X.

AU - Brandeker, A.

AU - Cabrera, J.

AU - Charnoz, S.

AU - Collier Cameron, A.

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 - Erikson, A.

AU - Fortier, A.

AU - Fossati, L.

AU - Fridlund, M.

AU - Gandolfi, D.

AU - Gillon, M.

AU - Güdel, M.

AU - Isaak, K.~G.

AU - Kiss, L.~L.

AU - Laskar, J.

AU - Lecavelier des Etangs, A.

AU - Lendl, M.

AU - Lovis, C.

AU - Luque, R.

AU - Magrin, D.

AU - Maxted, P.~F.~L.

AU - Mordasini, C.

AU - Olofsson, G.

AU - Ottensamer, R.

AU - Pallé, E.

AU - Peter, G.

AU - Piazza, D.

AU - Pollacco, D.

AU - Queloz, D.

AU - Ragazzoni, R.

AU - Rando, N.

AU - Ratti, F.

AU - Rauer, H.

AU - Ribas, I.

AU - Santos, N.~C.

AU - Scandariato, G.

AU - Ségransan, D.

AU - Simon, A.~E.

AU - Smith, A.~M.~S.

AU - Steinberger, M.

AU - Steller, M.

AU - Szabó, Gy. M.

AU - Thomas, N.

AU - Udry, S.

AU - Venturini, J.

AU - Walton, N.~A.

AU - Wolter, D.

PY - 2023/5/1

Y1 - 2023/5/1

N2 - Among the hundreds of known hot Jupiters (HJs), only five have been found to have companions on short-period orbits. Within this rare class of multiple planetary systems, the architecture of WASP-47 is unique, hosting an HJ (planet-b) with both an inner and an outer sub-Neptunian mass companion (-e and -d, respectively) as well as an additional non-transiting, long-period giant (-c). The small period ratio between planets -b and -d boosts the transit time variation (TTV) signal, making it possible to reliably measure the masses of these planets in synergy with the radial velocity (RV) technique. In this paper, we present new space- and ground-based photometric data of WASP-47b and WASP-47-d, including 11 unpublished light curves from the ESA mission CHaracterising ExOPlanet Satellite (CHEOPS). We analyzed the light curves in a homogeneous way together with all the publicly available data to carry out a global N-body dynamical modeling of the TTV and RV signals. We retrieved, among other parameters, a mass and density for planet -d of Md = 15.5 ± 0.8 M⊕ and ρd = 1.69 ± 0.22 g cm−3, which is in good agreement with the literature and consistent with a Neptune-like composition. For the inner planet (-e), we found a mass and density of Me = 9.0 ± 0.5 M⊕ and ρe = 8.1 ± 0.5 g cm−3, suggesting an Earth-like composition close to other ultra-hot planets at similar irradiation levels. Though this result is in agreement with previous RV plus TTV studies, it is not in agreement with the most recent RV analysis (at 2.8σ), which yielded a lower density compatible with a pure silicate composition. This discrepancy highlights the still unresolved issue of suspected systematic offsets between RV and TTV measurements. In this paper, we also significantly improve the orbital ephemerides of all transiting planets, which will be crucial for any future follow-up.

AB - Among the hundreds of known hot Jupiters (HJs), only five have been found to have companions on short-period orbits. Within this rare class of multiple planetary systems, the architecture of WASP-47 is unique, hosting an HJ (planet-b) with both an inner and an outer sub-Neptunian mass companion (-e and -d, respectively) as well as an additional non-transiting, long-period giant (-c). The small period ratio between planets -b and -d boosts the transit time variation (TTV) signal, making it possible to reliably measure the masses of these planets in synergy with the radial velocity (RV) technique. In this paper, we present new space- and ground-based photometric data of WASP-47b and WASP-47-d, including 11 unpublished light curves from the ESA mission CHaracterising ExOPlanet Satellite (CHEOPS). We analyzed the light curves in a homogeneous way together with all the publicly available data to carry out a global N-body dynamical modeling of the TTV and RV signals. We retrieved, among other parameters, a mass and density for planet -d of Md = 15.5 ± 0.8 M⊕ and ρd = 1.69 ± 0.22 g cm−3, which is in good agreement with the literature and consistent with a Neptune-like composition. For the inner planet (-e), we found a mass and density of Me = 9.0 ± 0.5 M⊕ and ρe = 8.1 ± 0.5 g cm−3, suggesting an Earth-like composition close to other ultra-hot planets at similar irradiation levels. Though this result is in agreement with previous RV plus TTV studies, it is not in agreement with the most recent RV analysis (at 2.8σ), which yielded a lower density compatible with a pure silicate composition. This discrepancy highlights the still unresolved issue of suspected systematic offsets between RV and TTV measurements. In this paper, we also significantly improve the orbital ephemerides of all transiting planets, which will be crucial for any future follow-up.

KW - techniques: photometric

KW - planets and satellites: detection

KW - planets and satellites: general

KW - Astrophysics - Earth and Planetary Astrophysics

KW - Astrophysics - Solar and Stellar Astrophysics

U2 - 10.1051/0004-6361/202245486

DO - 10.1051/0004-6361/202245486

M3 - Article

SN - 1432-0746

VL - 673

JO - Astronomy & Astrophysics

JF - Astronomy & Astrophysics

M1 - A42

ER -

A new dynamical modeling of the WASP-47 system with CHEOPS observations

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Subject classification (UKÄ)

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Projects

Consolidating CHEOPS and preparing for PLATO: Exoplanet studies in the 2020s

Cite this