A CHEOPS-enhanced view of the HD 3167 system

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Standard

A CHEOPS-enhanced view of the HD 3167 system. / Bourrier, V.; Deline, A.; Krenn, A.; Egger, J. A.; Petit, A. C.; Malavolta, L.; Cretignier, M.; Billot, N.; Broeg, C.; Florén, H.-G.; Queloz, D.; Alibert, Y.; Bonfanti, A.; Bonomo, A. S.; Delisle, J.-B.; Demangeon, O. D. S.; Demory, B.-O.; Dumusque, X.; Ehrenreich, D.; Haywood, R. D.; Howell, S. B.; Lendl, M.; Mortier, A.; Nigro, G.; Salmon, S.; Sousa, S. G.; Wilson, T. G.; Adibekyan, V.; Alonso, R.; Anglada, G.; Bárczy, T.; Navascues, D. Barrado y; Barros, S. C. C.; Baumjohann, W.; Beck, M.; Benz, W.; Biondi, F.; Bonfils, X.; Brandeker, A.; Cabrera, J.; Charnoz, S.; Csizmadia, Sz.; Cameron, A. Collier; Damasso, M.; Davies, M. B.; Deleuil, M.; Delrez, L.; Di Fabrizio, L.; Erikson, A.; Fortier, A.; Fossati, L.; Fridlund, M.; Gandolfi, D.; Gillon, M.; Güdel, M.; Heng, K.; Hoyer, S.; Isaak, K. G.; Kiss, L. L.; Laskar, J.; des Etangs, A. Lecavelier; Lorenzi, V.; Lovis, C.; Magrin, D.; Massa, A.; Maxted, P. F. L.; Nascimbeni, V.; Olofsson, G.; Ottensamer, R.; Pagano, I.; Pallé, E.; Peter, G.; Piotto, G.; Pollacco, D.; Ragazzoni, R.; Rando, N.; Rauer, H.; Ribas, I.; Santos, N. C.; Scandariato, G.; Ségransan, D.; Simon, A. E.; Smith, A. M. S.; Steller, M.; Szabó, Gy M.; Thomas, N.; Udry, S.; Van Grootel, V.; Verrecchia, F.; Walton, N.; Beck, T.; Buder, M.; Ratti, F.; Ulmer, B.; Viotto, V.

In: Astronomy and Astrophysics, Vol. 668, A31, 2022.

Research output: Contribution to journal › Journal article › Research › peer-review

Harvard

Bourrier, V, Deline, A, Krenn, A, Egger, JA, Petit, AC, Malavolta, L, Cretignier, M, Billot, N, Broeg, C, Florén, H-G, Queloz, D, Alibert, Y, Bonfanti, A, Bonomo, AS, Delisle, J-B, Demangeon, ODS, Demory, B-O, Dumusque, X, Ehrenreich, D, Haywood, RD, Howell, SB, Lendl, M, Mortier, A, Nigro, G, Salmon, S, Sousa, SG, Wilson, TG, Adibekyan, V, Alonso, R, Anglada, G, Bárczy, T, Navascues, DBY, Barros, SCC, Baumjohann, W, Beck, M, Benz, W, Biondi, F, Bonfils, X, Brandeker, A, Cabrera, J, Charnoz, S, Csizmadia, S, Cameron, AC, Damasso, M, Davies, MB, Deleuil, M, Delrez, L, Di Fabrizio, L, Erikson, A, Fortier, A, Fossati, L, Fridlund, M, Gandolfi, D, Gillon, M, Güdel, M, Heng, K, Hoyer, S, Isaak, KG, Kiss, LL, Laskar, J, des Etangs, AL, Lorenzi, V, Lovis, C, Magrin, D, Massa, A, Maxted, PFL, Nascimbeni, V, Olofsson, G, Ottensamer, R, Pagano, I, Pallé, E, Peter, G, Piotto, G, Pollacco, D, Ragazzoni, R, Rando, N, Rauer, H, Ribas, I, Santos, NC, Scandariato, G, Ségransan, D, Simon, AE, Smith, AMS, Steller, M, Szabó, GM, Thomas, N, Udry, S, Van Grootel, V, Verrecchia, F, Walton, N, Beck, T, Buder, M, Ratti, F, Ulmer, B & Viotto, V 2022, 'A CHEOPS-enhanced view of the HD 3167 system', Astronomy and Astrophysics, vol. 668, A31. https://doi.org/10.1051/0004-6361/202243778

APA

Bourrier, V., Deline, A., Krenn, A., Egger, J. A., Petit, A. C., Malavolta, L., Cretignier, M., Billot, N., Broeg, C., Florén, H-G., Queloz, D., Alibert, Y., Bonfanti, A., Bonomo, A. S., Delisle, J-B., Demangeon, O. D. S., Demory, B-O., Dumusque, X., Ehrenreich, D., ... Viotto, V. (2022). A CHEOPS-enhanced view of the HD 3167 system. Astronomy and Astrophysics, 668, [A31]. https://doi.org/10.1051/0004-6361/202243778

Vancouver

Bourrier V, Deline A, Krenn A, Egger JA, Petit AC, Malavolta L et al. A CHEOPS-enhanced view of the HD 3167 system. Astronomy and Astrophysics. 2022;668. A31. https://doi.org/10.1051/0004-6361/202243778

Author

Bourrier, V. ; Deline, A. ; Krenn, A. ; Egger, J. A. ; Petit, A. C. ; Malavolta, L. ; Cretignier, M. ; Billot, N. ; Broeg, C. ; Florén, H.-G. ; Queloz, D. ; Alibert, Y. ; Bonfanti, A. ; Bonomo, A. S. ; Delisle, J.-B. ; Demangeon, O. D. S. ; Demory, B.-O. ; Dumusque, X. ; Ehrenreich, D. ; Haywood, R. D. ; Howell, S. B. ; Lendl, M. ; Mortier, A. ; Nigro, G. ; Salmon, S. ; Sousa, S. G. ; Wilson, T. G. ; Adibekyan, V. ; Alonso, R. ; Anglada, G. ; Bárczy, T. ; Navascues, D. Barrado y ; Barros, S. C. C. ; Baumjohann, W. ; Beck, M. ; Benz, W. ; Biondi, F. ; Bonfils, X. ; Brandeker, A. ; Cabrera, J. ; Charnoz, S. ; Csizmadia, Sz. ; Cameron, A. Collier ; Damasso, M. ; Davies, M. B. ; Deleuil, M. ; Delrez, L. ; Di Fabrizio, L. ; Erikson, A. ; Fortier, A. ; Fossati, L. ; Fridlund, M. ; Gandolfi, D. ; Gillon, M. ; Güdel, M. ; Heng, K. ; Hoyer, S. ; Isaak, K. G. ; Kiss, L. L. ; Laskar, J. ; des Etangs, A. Lecavelier ; Lorenzi, V. ; Lovis, C. ; Magrin, D. ; Massa, A. ; Maxted, P. F. L. ; Nascimbeni, V. ; Olofsson, G. ; Ottensamer, R. ; Pagano, I. ; Pallé, E. ; Peter, G. ; Piotto, G. ; Pollacco, D. ; Ragazzoni, R. ; Rando, N. ; Rauer, H. ; Ribas, I. ; Santos, N. C. ; Scandariato, G. ; Ségransan, D. ; Simon, A. E. ; Smith, A. M. S. ; Steller, M. ; Szabó, Gy M. ; Thomas, N. ; Udry, S. ; Van Grootel, V. ; Verrecchia, F. ; Walton, N. ; Beck, T. ; Buder, M. ; Ratti, F. ; Ulmer, B. ; Viotto, V. / A CHEOPS-enhanced view of the HD 3167 system. In: Astronomy and Astrophysics. 2022 ; Vol. 668.

Bibtex

@article{3254bebe8b3944659c72bff81605adec,

title = "A CHEOPS-enhanced view of the HD 3167 system",

abstract = "Much remains to be understood about the nature of exoplanets smaller than Neptune, most of which have been discovered in compact multi-planet systems. With its inner ultra-short period planet b aligned with the star and two larger outer planets d-c on polar orbits, the multi-planet system HD 3167 features a peculiar architecture and offers the possibility to investigate both dynamical and atmospheric evolution processes. To this purpose we combined multiple datasets of transit photometry and radial velocimetry (RV) to revise the properties of the system and inform models of its planets. This effort was spearheaded by CHEOPS observations of HD 3167b, which appear inconsistent with a purely rocky composition despite its extreme irradiation. Overall the precision on the planetary orbital periods are improved by an order of magnitude, and the uncertainties on the densities of the transiting planets b and c are decreased by a factor of 3. Internal structure and atmospheric simulations draw a contrasting picture between HD 3167d, likely a rocky super-Earth that lost its atmosphere through photo-evaporation, and HD 3167c, a mini-Neptune that kept a substantial primordial gaseous envelope. We detect a fourth, more massive planet on a larger orbit, likely coplanar with HD 3167d-c. Dynamical simulations indeed show that the outer planetary system d-c-e was tilted, as a whole, early in the system history, when HD 3167b was still dominated by the star influence and maintained its aligned orbit. RV data and direct imaging rule out that the companion that could be responsible for the present-day architecture is still bound to the HD 3167 system. Similar global studies of multi-planet systems will tell how many share the peculiar properties of the HD 3167 system, which remains a target of choice for follow-up observations and simulations. ",

keywords = "Planet-star interactions, Planets and satellites: dynamical evolution and stability, Planets and satellites: individual: HD 3167, Planets and satellites: physical evolution, Techniques: photometric, Techniques: radial velocities",

author = "V. Bourrier and A. Deline and A. Krenn and Egger, {J. A.} and Petit, {A. C.} and L. Malavolta and M. Cretignier and N. Billot and C. Broeg and H.-G. Flor{\'e}n and D. Queloz and Y. Alibert and A. Bonfanti and Bonomo, {A. S.} and J.-B. Delisle and Demangeon, {O. D. S.} and B.-O. Demory and X. Dumusque and D. Ehrenreich and Haywood, {R. D.} and Howell, {S. B.} and M. Lendl and A. Mortier and G. Nigro and S. Salmon and Sousa, {S. G.} and Wilson, {T. G.} and V. Adibekyan and R. Alonso and G. Anglada and T. B{\'a}rczy and Navascues, {D. Barrado y} and Barros, {S. C. C.} and W. Baumjohann and M. Beck and W. Benz and F. Biondi and X. Bonfils and A. Brandeker and J. Cabrera and S. Charnoz and Sz. Csizmadia and Cameron, {A. Collier} and M. Damasso and Davies, {M. B.} and M. Deleuil and L. Delrez and {Di Fabrizio}, L. 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. Heng and S. Hoyer and Isaak, {K. G.} and Kiss, {L. L.} and J. Laskar and {des Etangs}, {A. Lecavelier} and V. Lorenzi and C. Lovis and D. Magrin and A. Massa and Maxted, {P. F. L.} and V. Nascimbeni and G. Olofsson and R. Ottensamer and I. Pagano and E. Pall{\'e} and G. Peter and G. Piotto and D. Pollacco and R. Ragazzoni and N. Rando and H. Rauer and I. Ribas and Santos, {N. C.} 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 {Van Grootel}, V. and F. Verrecchia and N. Walton and T. Beck and M. Buder and F. Ratti and B. Ulmer and V. Viotto",

year = "2022",

doi = "10.1051/0004-6361/202243778",

language = "English",

volume = "668",

journal = "Astronomy & Astrophysics",

issn = "0004-6361",

publisher = "E D P Sciences",

}

RIS

TY - JOUR

T1 - A CHEOPS-enhanced view of the HD 3167 system

AU - Bourrier, V.

AU - Deline, A.

AU - Krenn, A.

AU - Egger, J. A.

AU - Petit, A. C.

AU - Malavolta, L.

AU - Cretignier, M.

AU - Billot, N.

AU - Broeg, C.

AU - Florén, H.-G.

AU - Queloz, D.

AU - Alibert, Y.

AU - Bonfanti, A.

AU - Bonomo, A. S.

AU - Delisle, J.-B.

AU - Demangeon, O. D. S.

AU - Demory, B.-O.

AU - Dumusque, X.

AU - Ehrenreich, D.

AU - Haywood, R. D.

AU - Howell, S. B.

AU - Lendl, M.

AU - Mortier, A.

AU - Nigro, G.

AU - Salmon, S.

AU - Sousa, S. G.

AU - Wilson, T. G.

AU - Adibekyan, V.

AU - Alonso, R.

AU - Anglada, G.

AU - Bárczy, T.

AU - Navascues, D. Barrado y

AU - Barros, S. C. C.

AU - Baumjohann, W.

AU - Beck, M.

AU - Benz, W.

AU - Biondi, F.

AU - Bonfils, X.

AU - Brandeker, A.

AU - Cabrera, J.

AU - Charnoz, S.

AU - Csizmadia, Sz.

AU - Cameron, A. Collier

AU - Damasso, M.

AU - Davies, M. B.

AU - Deleuil, M.

AU - Delrez, L.

AU - Di Fabrizio, L.

AU - Erikson, A.

AU - Fortier, A.

AU - Fossati, L.

AU - Fridlund, M.

AU - Gandolfi, D.

AU - Gillon, M.

AU - Güdel, M.

AU - Heng, K.

AU - Hoyer, S.

AU - Isaak, K. G.

AU - Kiss, L. L.

AU - Laskar, J.

AU - des Etangs, A. Lecavelier

AU - Lorenzi, V.

AU - Lovis, C.

AU - Magrin, D.

AU - Massa, A.

AU - Maxted, P. F. L.

AU - Nascimbeni, V.

AU - Olofsson, G.

AU - Ottensamer, R.

AU - Pagano, I.

AU - Pallé, E.

AU - Peter, G.

AU - Piotto, G.

AU - Pollacco, D.

AU - Ragazzoni, R.

AU - Rando, N.

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 - Steller, M.

AU - Szabó, Gy M.

AU - Thomas, N.

AU - Udry, S.

AU - Van Grootel, V.

AU - Verrecchia, F.

AU - Walton, N.

AU - Beck, T.

AU - Buder, M.

AU - Ratti, F.

AU - Ulmer, B.

AU - Viotto, V.

PY - 2022

Y1 - 2022

N2 - Much remains to be understood about the nature of exoplanets smaller than Neptune, most of which have been discovered in compact multi-planet systems. With its inner ultra-short period planet b aligned with the star and two larger outer planets d-c on polar orbits, the multi-planet system HD 3167 features a peculiar architecture and offers the possibility to investigate both dynamical and atmospheric evolution processes. To this purpose we combined multiple datasets of transit photometry and radial velocimetry (RV) to revise the properties of the system and inform models of its planets. This effort was spearheaded by CHEOPS observations of HD 3167b, which appear inconsistent with a purely rocky composition despite its extreme irradiation. Overall the precision on the planetary orbital periods are improved by an order of magnitude, and the uncertainties on the densities of the transiting planets b and c are decreased by a factor of 3. Internal structure and atmospheric simulations draw a contrasting picture between HD 3167d, likely a rocky super-Earth that lost its atmosphere through photo-evaporation, and HD 3167c, a mini-Neptune that kept a substantial primordial gaseous envelope. We detect a fourth, more massive planet on a larger orbit, likely coplanar with HD 3167d-c. Dynamical simulations indeed show that the outer planetary system d-c-e was tilted, as a whole, early in the system history, when HD 3167b was still dominated by the star influence and maintained its aligned orbit. RV data and direct imaging rule out that the companion that could be responsible for the present-day architecture is still bound to the HD 3167 system. Similar global studies of multi-planet systems will tell how many share the peculiar properties of the HD 3167 system, which remains a target of choice for follow-up observations and simulations.

AB - Much remains to be understood about the nature of exoplanets smaller than Neptune, most of which have been discovered in compact multi-planet systems. With its inner ultra-short period planet b aligned with the star and two larger outer planets d-c on polar orbits, the multi-planet system HD 3167 features a peculiar architecture and offers the possibility to investigate both dynamical and atmospheric evolution processes. To this purpose we combined multiple datasets of transit photometry and radial velocimetry (RV) to revise the properties of the system and inform models of its planets. This effort was spearheaded by CHEOPS observations of HD 3167b, which appear inconsistent with a purely rocky composition despite its extreme irradiation. Overall the precision on the planetary orbital periods are improved by an order of magnitude, and the uncertainties on the densities of the transiting planets b and c are decreased by a factor of 3. Internal structure and atmospheric simulations draw a contrasting picture between HD 3167d, likely a rocky super-Earth that lost its atmosphere through photo-evaporation, and HD 3167c, a mini-Neptune that kept a substantial primordial gaseous envelope. We detect a fourth, more massive planet on a larger orbit, likely coplanar with HD 3167d-c. Dynamical simulations indeed show that the outer planetary system d-c-e was tilted, as a whole, early in the system history, when HD 3167b was still dominated by the star influence and maintained its aligned orbit. RV data and direct imaging rule out that the companion that could be responsible for the present-day architecture is still bound to the HD 3167 system. Similar global studies of multi-planet systems will tell how many share the peculiar properties of the HD 3167 system, which remains a target of choice for follow-up observations and simulations.

KW - Planet-star interactions

KW - Planets and satellites: dynamical evolution and stability

KW - Planets and satellites: individual: HD 3167

KW - Planets and satellites: physical evolution

KW - Techniques: photometric

KW - Techniques: radial velocities

U2 - 10.1051/0004-6361/202243778

DO - 10.1051/0004-6361/202243778

M3 - Journal article

AN - SCOPUS:85145347243

VL - 668

JO - Astronomy & Astrophysics

JF - Astronomy & Astrophysics

SN - 0004-6361

M1 - A31

ER -

ID: 339260270

Globe Institute