TOI-1055 b: Neptunian planet characterised with HARPS, TESS, and CHEOPS

A. Bonfanti; D. Gandolfi; J. A. Egger; L. Fossati; J. Cabrera; A. Krenn; Y. Alibert; W. Benz; N. Billot; H. G. Florén; M. Lendl; V. Adibekyan; S. Salmon; N. C. Santos; S. G. Sousa; T. G. Wilson; O. Barragán; A. Collier Cameron; L. Delrez; M. Esposito; E. Goffo; H. Osborne; H. P. Osborn; L. M. Serrano; V. Van Eylen; J. Alarcon; R. Alonso; G. Anglada; T. Bárczy; D. Barrado Navascues; S. C.C. Barros; W. Baumjohann; M. Beck; T. Beck; M. Bedell; X. Bonfils; L. Borsato; A. Brandeker; C. Broeg; S. Charnoz; C. Corral Van Damme; Sz Csizmadia; P. E. Cubillos; M. B. Davies; M. Deleuil; O. D.S. Demangeon; B. O. Demory; D. Ehrenreich; A. Erikson; A. Fortier; M. Fridlund; M. Gillon; M. Güdel; S. Hoyer; K. G. Isaak; F. Kerschbaum; L. L. Kiss; J. Laskar; A. Lecavelier Des Etangs; D. Lorenzo-Oliveira; C. Lovis; D. Magrin; L. Marafatto; P. F.L. Maxted; J. Meléndez; C. Mordasini; 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; G. Scandariato; D. Ségransan; A. E. Simon; A. M.S. Smith; M. Steller; Gy M. Szabó; N. Thomas; S. Udry; B. Ulmer; V. Van Grootel; J. Venturini; N. A. Walton

doi:10.1051/0004-6361/202245607

TOI-1055 b: Neptunian planet characterised with HARPS, TESS, and CHEOPS

A. Bonfanti
, D. Gandolfi
, J. A. Egger
, L. Fossati
, J. Cabrera
, A. Krenn
, Y. Alibert
, W. Benz
, N. Billot
, H. G. Florén
, M. Lendl
, V. Adibekyan
, S. Salmon
, N. C. Santos
, S. G. Sousa
, T. G. Wilson
, O. Barragán
, A. Collier Cameron
, L. Delrez
, M. Esposito

E. Goffo, H. Osborne, H. P. Osborn, L. M. Serrano, V. Van Eylen, J. Alarcon, R. Alonso, G. Anglada, T. Bárczy, D. Barrado Navascues, S. C.C. Barros, W. Baumjohann, M. Beck, T. Beck, M. Bedell, X. Bonfils, L. Borsato, A. Brandeker, C. Broeg, S. Charnoz, C. Corral Van Damme, Sz Csizmadia, P. E. Cubillos, M. B. Davies, M. Deleuil, O. D.S. Demangeon, B. O. Demory, D. Ehrenreich, A. Erikson, A. Fortier, M. Fridlund, M. Gillon, M. Güdel, S. Hoyer, K. G. Isaak, F. Kerschbaum, L. L. Kiss, J. Laskar, A. Lecavelier Des Etangs, D. Lorenzo-Oliveira, C. Lovis, D. Magrin, L. Marafatto, P. F.L. Maxted, J. Meléndez, C. Mordasini, 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, G. Scandariato, D. Ségransan, A. E. Simon, A. M.S. Smith, M. Steller, Gy M. Szabó, N. Thomas, S. Udry, B. Ulmer, V. Van Grootel, J. Venturini, N. A. Walton

Space Research Institute
Dipartimento di Fisica
University of Turin
University of Bern
DLR
Center for Space and Habitability
Université de Genève
Department of Astronomy
Stockholm University
Ipatimup Diagnósticos
Departamento de Fisica e Astronomia
University of St Andrews
Sub-department of Astrophysics
University of Oxford
Astrobiology Research Unit
University of Liège
Thüringer Landessternwarte Tautenburg
UCL Mullard Space Science Laboratory
Department of Physics
Massachusetts Institute of Technology
European Southern Observatory Santiago
Instituto de Astrofisica de Canarias
Departamento de Astrofisica
Research Unit; CIBERNED and Universidad de La Laguna
Institut de Ciencies de l’Espai (ICE
Campus UAB
Institut d’Estudis Espacials de Catalunya (IEEC)
Admatis Ltd.
Depto. de Astrofisica
ESAC campus
Center for Computational Astrophysics
Flatiron Institute
Université Grenoble Alpes
INAF Osservatorio Astronomico di Padova
Center for Space and Habitability
Université Paris Diderot
ESTEC - European Space Research and Technology Centre
Istituto di Astrofisica e Planetologia Spaziali (IAPS)
Lund University
LAM
University of Leiden
Department of Space
Onsala Space Observatory
Department of Astrophysics
University of Vienna
Science and Operations Department - Science Division (SCI-SC)
Konkoly Observatory
Institute of Physics
Eötvös Loránd University
Sorbonne Univ.
Institut d’Astrophysique de Paris
Laboratório Nacional de Astrofísica
Department of Astronomy
University of São Paulo
Astrophysics Group
Keele University
INAF Osservatorio Astrofisico di Catania
Institute of Optical Sensor Systems
University of Padova
University of Warwick
Department of Physics
University of Cambridge
Zentrum für Astronomie und Astrophysik
TU Berlin
Free University of Berlin
Institute of Astronomy
University of Geneva
ETH Zurich

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

7 Citations (Scopus)

Abstract

Context. TOI-1055 is a Sun-like star known to host a transiting Neptune-sized planet on a 17.5-day orbit (TOI-1055 b). Radial velocity (RV) analyses carried out by two independent groups using nearly the same set of HARPS spectra have provided measurements of planetary masses that differ by ∼2σ. Aims. Our aim in this work is to solve the inconsistency in the published planetary masses by significantly extending the set of HARPS RV measurements and employing a new analysis tool that is able to account and correct for stellar activity. Our further aim was to improve the precision on measurements of the planetary radius by observing two transits of the planet with the CHEOPS space telescope. Methods. We fit a skew normal function to each cross correlation function extracted from the HARPS spectra to obtain RV measurements and hyperparameters to be used for the detrending. We evaluated the correlation changes of the hyperparameters along the RV time series using the breakpoint technique. We performed a joint photometric and RV analysis using a Markov chain Monte Carlo scheme to simultaneously detrend the light curves and the RV time series. Results. We firmly detected the Keplerian signal of TOI-1055 b, deriving a planetary mass of Mb = 20.4-2.5+2.6 MO (∼12%). This value is in agreement with one of the two estimates in the literature, but it is significantly more precise. Thanks to the TESS transit light curves combined with exquisite CHEOPS photometry, we also derived a planetary radius of Rb = 3.490-0.064+0.070 RO (∼1.9%). Our mass and radius measurements imply a mean density of ρb = 2.65-0.35+0.37 g cm-3 (∼14%). We further inferred the planetary structure and found that TOI-1055 b is very likely to host a substantial gas envelope with a mass of 0.41-0.20+0.34 MO and a thickness of 1.05-0.29+0.30 RO. Conclusions. Our RV extraction combined with the breakpoint technique has played a key role in the optimal removal of stellar activity from the HARPS time series, enabling us to solve the tension in the planetary mass values published so far for TOI-1055 b.

Original language	English
Article number	L8
Journal	Astronomy and Astrophysics
Volume	671
DOIs	https://doi.org/10.1051/0004-6361/202245607
Publication status	Published - 1 Mar 2023
Externally published	Yes

Keywords

Planets and satellites: fundamental parameters
Stars: fundamental parameters
Techniques: photometric
Techniques: radial velocities

Access to Document

10.1051/0004-6361/202245607

Cite this

Bonfanti, A., Gandolfi, D., Egger, J. A., Fossati, L., Cabrera, J., Krenn, A., Alibert, Y., Benz, W., Billot, N., Florén, H. G., Lendl, M., Adibekyan, V., Salmon, S., Santos, N. C., Sousa, S. G., Wilson, T. G., Barragán, O., Collier Cameron, A., Delrez, L., ... Walton, N. A. (2023). TOI-1055 b: Neptunian planet characterised with HARPS, TESS, and CHEOPS. Astronomy and Astrophysics, 671, Article L8. https://doi.org/10.1051/0004-6361/202245607

@article{28a998922d774a39b07c97f437bdd0d6,

title = "TOI-1055 b: Neptunian planet characterised with HARPS, TESS, and CHEOPS",

abstract = "Context. TOI-1055 is a Sun-like star known to host a transiting Neptune-sized planet on a 17.5-day orbit (TOI-1055 b). Radial velocity (RV) analyses carried out by two independent groups using nearly the same set of HARPS spectra have provided measurements of planetary masses that differ by ∼2σ. Aims. Our aim in this work is to solve the inconsistency in the published planetary masses by significantly extending the set of HARPS RV measurements and employing a new analysis tool that is able to account and correct for stellar activity. Our further aim was to improve the precision on measurements of the planetary radius by observing two transits of the planet with the CHEOPS space telescope. Methods. We fit a skew normal function to each cross correlation function extracted from the HARPS spectra to obtain RV measurements and hyperparameters to be used for the detrending. We evaluated the correlation changes of the hyperparameters along the RV time series using the breakpoint technique. We performed a joint photometric and RV analysis using a Markov chain Monte Carlo scheme to simultaneously detrend the light curves and the RV time series. Results. We firmly detected the Keplerian signal of TOI-1055 b, deriving a planetary mass of Mb = 20.4-2.5+2.6 MO (∼12\%). This value is in agreement with one of the two estimates in the literature, but it is significantly more precise. Thanks to the TESS transit light curves combined with exquisite CHEOPS photometry, we also derived a planetary radius of Rb = 3.490-0.064+0.070 RO (∼1.9\%). Our mass and radius measurements imply a mean density of ρb = 2.65-0.35+0.37 g cm-3 (∼14\%). We further inferred the planetary structure and found that TOI-1055 b is very likely to host a substantial gas envelope with a mass of 0.41-0.20+0.34 MO and a thickness of 1.05-0.29+0.30 RO. Conclusions. Our RV extraction combined with the breakpoint technique has played a key role in the optimal removal of stellar activity from the HARPS time series, enabling us to solve the tension in the planetary mass values published so far for TOI-1055 b.",

keywords = "Planets and satellites: fundamental parameters, Stars: fundamental parameters, Techniques: photometric, Techniques: radial velocities",

author = "A. Bonfanti and D. Gandolfi and Egger, \{J. A.\} and L. Fossati and J. Cabrera and A. Krenn and Y. Alibert and W. Benz and N. Billot and Flor{\'e}n, \{H. G.\} and M. Lendl and V. Adibekyan and S. Salmon and Santos, \{N. C.\} and Sousa, \{S. G.\} and Wilson, \{T. G.\} and O. Barrag{\'a}n and \{Collier Cameron\}, A. and L. Delrez and M. Esposito and E. Goffo and H. Osborne and Osborn, \{H. P.\} and Serrano, \{L. M.\} and \{Van Eylen\}, V. and J. Alarcon and R. Alonso and G. Anglada and T. B{\'a}rczy and \{Barrado Navascues\}, D. and Barros, \{S. C.C.\} and W. Baumjohann and M. Beck and T. Beck and M. Bedell and X. Bonfils and L. Borsato and A. Brandeker and C. Broeg and S. Charnoz and \{Corral Van Damme\}, C. and Sz Csizmadia and Cubillos, \{P. E.\} and Davies, \{M. B.\} and M. Deleuil and Demangeon, \{O. D.S.\} and Demory, \{B. O.\} and D. Ehrenreich and A. Erikson and A. Fortier and M. Fridlund and M. Gillon and M. G{\"u}del and S. Hoyer and Isaak, \{K. G.\} and F. Kerschbaum and Kiss, \{L. L.\} and J. Laskar and \{Lecavelier Des Etangs\}, A. and D. Lorenzo-Oliveira and C. Lovis and D. Magrin and L. Marafatto and Maxted, \{P. F.L.\} and J. Mel{\'e}ndez and C. Mordasini 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 G. Scandariato and D. S{\'e}gransan and Simon, \{A. E.\} and Smith, \{A. M.S.\} and M. Steller and Szab{\'o}, \{Gy M.\} and N. Thomas and S. Udry and B. Ulmer and \{Van Grootel\}, V. and J. Venturini and Walton, \{N. A.\}",

note = "Publisher Copyright: {\textcopyright} The Authors 2023.",

year = "2023",

month = mar,

day = "1",

doi = "10.1051/0004-6361/202245607",

language = "English",

volume = "671",

journal = "Astronomy and Astrophysics",

issn = "0004-6361",

publisher = "EDP Sciences",

}

Bonfanti, A, Gandolfi, D, Egger, JA, Fossati, L, Cabrera, J, Krenn, A, Alibert, Y, Benz, W, Billot, N, Florén, HG, Lendl, M, Adibekyan, V, Salmon, S, Santos, NC, Sousa, SG, Wilson, TG, Barragán, O, Collier Cameron, A, Delrez, L, Esposito, M, Goffo, E, Osborne, H, Osborn, HP, Serrano, LM, Van Eylen, V, Alarcon, J, Alonso, R, Anglada, G, Bárczy, T, Barrado Navascues, D, Barros, SCC, Baumjohann, W, Beck, M, Beck, T, Bedell, M, Bonfils, X, Borsato, L, Brandeker, A, Broeg, C, Charnoz, S, Corral Van Damme, C, Csizmadia, S, Cubillos, PE, Davies, MB, Deleuil, M, Demangeon, ODS, Demory, BO, Ehrenreich, D, Erikson, A, Fortier, A, Fridlund, M, Gillon, M, Güdel, M, Hoyer, S, Isaak, KG, Kerschbaum, F, Kiss, LL, Laskar, J, Lecavelier Des Etangs, A, Lorenzo-Oliveira, D, Lovis, C, Magrin, D, Marafatto, L, Maxted, PFL, Meléndez, J, Mordasini, C, 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, Scandariato, G, Ségransan, D, Simon, AE, Smith, AMS, Steller, M, Szabó, GM, Thomas, N, Udry, S, Ulmer, B, Van Grootel, V, Venturini, J & Walton, NA 2023, 'TOI-1055 b: Neptunian planet characterised with HARPS, TESS, and CHEOPS', Astronomy and Astrophysics, vol. 671, L8. https://doi.org/10.1051/0004-6361/202245607

TY - JOUR

T1 - TOI-1055 b

T2 - Neptunian planet characterised with HARPS, TESS, and CHEOPS

AU - Bonfanti, A.

AU - Gandolfi, D.

AU - Egger, J. A.

AU - Fossati, L.

AU - Cabrera, J.

AU - Krenn, A.

AU - Alibert, Y.

AU - Benz, W.

AU - Billot, N.

AU - Florén, H. G.

AU - Lendl, M.

AU - Adibekyan, V.

AU - Salmon, S.

AU - Santos, N. C.

AU - Sousa, S. G.

AU - Wilson, T. G.

AU - Barragán, O.

AU - Collier Cameron, A.

AU - Delrez, L.

AU - Esposito, M.

AU - Goffo, E.

AU - Osborne, H.

AU - Osborn, H. P.

AU - Serrano, L. M.

AU - Van Eylen, V.

AU - Alarcon, J.

AU - Alonso, R.

AU - Anglada, G.

AU - Bárczy, T.

AU - Barrado Navascues, D.

AU - Barros, S. C.C.

AU - Baumjohann, W.

AU - Beck, M.

AU - Beck, T.

AU - Bedell, M.

AU - Bonfils, X.

AU - Borsato, L.

AU - Brandeker, A.

AU - Broeg, C.

AU - Charnoz, S.

AU - Corral Van Damme, C.

AU - Csizmadia, Sz

AU - Cubillos, P. E.

AU - Davies, M. B.

AU - Deleuil, M.

AU - Demangeon, O. D.S.

AU - Demory, B. O.

AU - Ehrenreich, D.

AU - Erikson, A.

AU - Fortier, A.

AU - Fridlund, M.

AU - Gillon, M.

AU - Güdel, M.

AU - Hoyer, S.

AU - Isaak, K. G.

AU - Kerschbaum, F.

AU - Kiss, L. L.

AU - Laskar, J.

AU - Lecavelier Des Etangs, A.

AU - Lorenzo-Oliveira, D.

AU - Lovis, C.

AU - Magrin, D.

AU - Marafatto, L.

AU - Maxted, P. F.L.

AU - Meléndez, J.

AU - Mordasini, C.

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 - Scandariato, G.

AU - Ségransan, D.

AU - Simon, A. E.

AU - Smith, A. M.S.

AU - Steller, M.

AU - Szabó, Gy M.

AU - Thomas, N.

AU - Udry, S.

AU - Ulmer, B.

AU - Van Grootel, V.

AU - Venturini, J.

AU - Walton, N. A.

PY - 2023/3/1

Y1 - 2023/3/1

N2 - Context. TOI-1055 is a Sun-like star known to host a transiting Neptune-sized planet on a 17.5-day orbit (TOI-1055 b). Radial velocity (RV) analyses carried out by two independent groups using nearly the same set of HARPS spectra have provided measurements of planetary masses that differ by ∼2σ. Aims. Our aim in this work is to solve the inconsistency in the published planetary masses by significantly extending the set of HARPS RV measurements and employing a new analysis tool that is able to account and correct for stellar activity. Our further aim was to improve the precision on measurements of the planetary radius by observing two transits of the planet with the CHEOPS space telescope. Methods. We fit a skew normal function to each cross correlation function extracted from the HARPS spectra to obtain RV measurements and hyperparameters to be used for the detrending. We evaluated the correlation changes of the hyperparameters along the RV time series using the breakpoint technique. We performed a joint photometric and RV analysis using a Markov chain Monte Carlo scheme to simultaneously detrend the light curves and the RV time series. Results. We firmly detected the Keplerian signal of TOI-1055 b, deriving a planetary mass of Mb = 20.4-2.5+2.6 MO (∼12%). This value is in agreement with one of the two estimates in the literature, but it is significantly more precise. Thanks to the TESS transit light curves combined with exquisite CHEOPS photometry, we also derived a planetary radius of Rb = 3.490-0.064+0.070 RO (∼1.9%). Our mass and radius measurements imply a mean density of ρb = 2.65-0.35+0.37 g cm-3 (∼14%). We further inferred the planetary structure and found that TOI-1055 b is very likely to host a substantial gas envelope with a mass of 0.41-0.20+0.34 MO and a thickness of 1.05-0.29+0.30 RO. Conclusions. Our RV extraction combined with the breakpoint technique has played a key role in the optimal removal of stellar activity from the HARPS time series, enabling us to solve the tension in the planetary mass values published so far for TOI-1055 b.

AB - Context. TOI-1055 is a Sun-like star known to host a transiting Neptune-sized planet on a 17.5-day orbit (TOI-1055 b). Radial velocity (RV) analyses carried out by two independent groups using nearly the same set of HARPS spectra have provided measurements of planetary masses that differ by ∼2σ. Aims. Our aim in this work is to solve the inconsistency in the published planetary masses by significantly extending the set of HARPS RV measurements and employing a new analysis tool that is able to account and correct for stellar activity. Our further aim was to improve the precision on measurements of the planetary radius by observing two transits of the planet with the CHEOPS space telescope. Methods. We fit a skew normal function to each cross correlation function extracted from the HARPS spectra to obtain RV measurements and hyperparameters to be used for the detrending. We evaluated the correlation changes of the hyperparameters along the RV time series using the breakpoint technique. We performed a joint photometric and RV analysis using a Markov chain Monte Carlo scheme to simultaneously detrend the light curves and the RV time series. Results. We firmly detected the Keplerian signal of TOI-1055 b, deriving a planetary mass of Mb = 20.4-2.5+2.6 MO (∼12%). This value is in agreement with one of the two estimates in the literature, but it is significantly more precise. Thanks to the TESS transit light curves combined with exquisite CHEOPS photometry, we also derived a planetary radius of Rb = 3.490-0.064+0.070 RO (∼1.9%). Our mass and radius measurements imply a mean density of ρb = 2.65-0.35+0.37 g cm-3 (∼14%). We further inferred the planetary structure and found that TOI-1055 b is very likely to host a substantial gas envelope with a mass of 0.41-0.20+0.34 MO and a thickness of 1.05-0.29+0.30 RO. Conclusions. Our RV extraction combined with the breakpoint technique has played a key role in the optimal removal of stellar activity from the HARPS time series, enabling us to solve the tension in the planetary mass values published so far for TOI-1055 b.

KW - Planets and satellites: fundamental parameters

KW - Stars: fundamental parameters

KW - Techniques: photometric

KW - Techniques: radial velocities

U2 - 10.1051/0004-6361/202245607

DO - 10.1051/0004-6361/202245607

M3 - Article

AN - SCOPUS:85149928701

SN - 0004-6361

VL - 671

JO - Astronomy and Astrophysics

JF - Astronomy and Astrophysics

M1 - L8

ER -

TOI-1055 b: Neptunian planet characterised with HARPS, TESS, and CHEOPS

Abstract

Keywords

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