Uncovering the true periods of the young sub-Neptunes orbiting TOI-2076

H. P. Osborn; A. Bonfanti; D. Gandolfi; C. Hedges; A. Leleu; A. Fortier; D. Futyan; P. Gutermann; P. F.L. Maxted; L. Borsato; K. A. Collins; J. Gomes Da Silva; Y. Gomez Maqueo Chew; M. J. Hooton; M. Lendl; H. Parviainen; S. Salmon; N. Schanche; L. M. Serrano; S. G. Sousa; A. Tuson; S. Ulmer-Moll; V. Van Grootel; R. D. Wells; T. G. Wilson; Y. Alibert; R. Alonso; G. Anglada; J. Asquier; D. Barrado Y Navascues; W. Baumjohann; T. Beck; W. Benz; F. Biondi; X. Bonfils; F. Bouchy; A. Brandeker; C. Broeg; T. Barczy; S. C.C. Barros; J. Cabrera; S. Charnoz; A. Collier Cameron; S. Csizmadia; M. B. Davies; M. Deleuil; L. Delrez; B. O. Demory; D. Ehrenreich; A. Erikson; L. Fossati; M. Fridlund; M. Gillon; M. A. Gomez-Munoz; M. Gudel; K. Heng; S. Hoyer; K. G. Isaak; L. Kiss; J. Laskar; A. Lecavelier Des Etangs; C. Lovis; D. Magrin; L. Malavolta; J. McCormac; V. Nascimbeni; G. Olofsson; R. Ottensamer; I. Pagano; E. Palle; G. Peter; D. Piazza; G. Piotto; D. Pollacco; D. Queloz; R. Ragazzoni; N. Rando; H. Rauer; C. Reimers; I. Ribas; O. D.S. Demangeon; A. M.S. Smith; L. Sabin; N. Santos; G. Scandariato; U. Schroffenegger; R. P. Schwarz; A. Shporer; A. E. Simon; M. Steller; G. M. Szabo; D. Segransan; N. Thomas; S. Udry; I. Walter; N. Walton

doi:10.1051/0004-6361/202243065

Uncovering the true periods of the young sub-Neptunes orbiting TOI-2076

H. P. Osborn^*, A. Bonfanti, D. Gandolfi, C. Hedges, A. Leleu, A. Fortier, D. Futyan, P. Gutermann, P. F.L. Maxted, L. Borsato, K. A. Collins, J. Gomes Da Silva, Y. Gomez Maqueo Chew, M. J. Hooton, M. Lendl, H. Parviainen, S. Salmon, N. Schanche, L. M. Serrano, S. G. SousaA. Tuson, S. Ulmer-Moll, V. Van Grootel, R. D. Wells, T. G. Wilson, Y. Alibert, R. Alonso, G. Anglada, J. Asquier, D. Barrado Y Navascues, W. Baumjohann, T. Beck, W. Benz, F. Biondi, X. Bonfils, F. Bouchy, A. Brandeker, C. Broeg, T. Barczy, S. C.C. Barros, J. Cabrera, S. Charnoz, A. Collier Cameron, S. Csizmadia, M. B. Davies, M. Deleuil, L. Delrez, B. O. Demory, D. Ehrenreich, A. Erikson, L. Fossati, M. Fridlund, M. Gillon, M. A. Gomez-Munoz, M. Gudel, K. Heng, S. Hoyer, K. G. Isaak, L. Kiss, J. Laskar, A. Lecavelier Des Etangs, C. Lovis, D. Magrin, L. Malavolta, J. McCormac, V. Nascimbeni, G. Olofsson, R. Ottensamer, I. Pagano, E. Palle, G. Peter, D. Piazza, G. Piotto, D. Pollacco, D. Queloz, R. Ragazzoni, N. Rando, H. Rauer, C. Reimers, I. Ribas, O. D.S. Demangeon, A. M.S. Smith, L. Sabin, N. Santos, G. Scandariato, U. Schroffenegger, R. P. Schwarz, A. Shporer, A. E. Simon, M. Steller, G. M. Szabo, D. Segransan, N. Thomas, S. Udry, I. Walter, N. Walton

^*Corresponding author for this work

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

Abstract

Context. TOI-2076 is a transiting three-planet system of sub-Neptunes orbiting a bright (G = 8.9 mag), young (340 ±80 Myr) K-type star. Although a validated planetary system, the orbits of the two outer planets were unconstrained as only two non-consecutive transits were seen in TESS photometry. This left 11 and 7 possible period aliases for each.

Aims. To reveal the true orbits of these two long-period planets, precise photometry targeted on the highest-probability period aliases is required. Long-term monitoring of transits in multi-planet systems can also help constrain planetary masses through TTV measurements.

Methods. We used the MonoTools package to determine which aliases to follow, and then performed space-based and ground-based photometric follow-up of TOI-2076 c and d with CHEOPS, SAINT-EX, and LCO telescopes.

Results. CHEOPS observations revealed a clear detection for TOI-2076 c at P = 21.01538^+0.00084_-0.00074 d, and allowed us to rule out three of the most likely period aliases for TOI-2076 d. Ground-based photometry further enabled us to rule out remaining aliases and confirm the P = 35.12537 ±0.00067 d alias. These observations also improved the radius precision of all three sub-Neptunes to 2.518 ±0.036, 3.497 ±0.043, and 3.232 ±0.063 R_⊕. Our observations also revealed a clear anti-correlated TTV signal between planets b and c likely caused by their proximity to the 2:1 resonance, while planets c and d appear close to a 5:3 period commensurability, although model degeneracy meant we were unable to retrieve robust TTV masses. Their inflated radii, likely due to extended H-He atmospheres, combined with low insolation makes all three planets excellent candidates for future comparative transmission spectroscopy with JWST.

Original language	English
Article number	A156
Number of pages	17
Journal	Astronomy and Astrophysics
Volume	664
Early online date	25 Aug 2022
DOIs	https://doi.org/10.1051/0004-6361/202243065
Publication status	Published - 25 Aug 2022

Keywords

Planets and satellites: detection
Stars: individual: TOI-2076
Techniques: photometric

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10.1051/0004-6361/202243065

Osborn_2022_AA_Uncovering-true_VoR
Copyright © ESO 2022. This work has been made available online in accordance with publisher policies or with permission. Permission for further reuse of this content should be sought from the publisher or the rights holder. This is the final published version of the work, which was originally published at https://doi.org/10.1051/0004-6361/202243065.
Final published version, 4.29 MBLicence: CC BY

https://arxiv.org/abs/2203.03194

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Osborn, H. P., Bonfanti, A., Gandolfi, D., Hedges, C., Leleu, A., Fortier, A., Futyan, D., Gutermann, P., Maxted, P. F. L., Borsato, L., Collins, K. A., Da Silva, J. G., Chew, Y. G. M., Hooton, M. J., Lendl, M., Parviainen, H., Salmon, S., Schanche, N., Serrano, L. M., ... Walton, N. (2022). Uncovering the true periods of the young sub-Neptunes orbiting TOI-2076. Astronomy and Astrophysics, 664, Article A156. https://doi.org/10.1051/0004-6361/202243065

@article{aca2ec669a8445559e0850ec8f2f26f6,

title = "Uncovering the true periods of the young sub-Neptunes orbiting TOI-2076",

abstract = "Context. TOI-2076 is a transiting three-planet system of sub-Neptunes orbiting a bright (G = 8.9 mag), young (340 ±80 Myr) K-type star. Although a validated planetary system, the orbits of the two outer planets were unconstrained as only two non-consecutive transits were seen in TESS photometry. This left 11 and 7 possible period aliases for each. Aims. To reveal the true orbits of these two long-period planets, precise photometry targeted on the highest-probability period aliases is required. Long-term monitoring of transits in multi-planet systems can also help constrain planetary masses through TTV measurements. Methods. We used the MonoTools package to determine which aliases to follow, and then performed space-based and ground-based photometric follow-up of TOI-2076 c and d with CHEOPS, SAINT-EX, and LCO telescopes. Results. CHEOPS observations revealed a clear detection for TOI-2076 c at P = 21.01538+0.00084 -0.00074 d, and allowed us to rule out three of the most likely period aliases for TOI-2076 d. Ground-based photometry further enabled us to rule out remaining aliases and confirm the P = 35.12537 ±0.00067 d alias. These observations also improved the radius precision of all three sub-Neptunes to 2.518 ±0.036, 3.497 ±0.043, and 3.232 ±0.063 R⊕. Our observations also revealed a clear anti-correlated TTV signal between planets b and c likely caused by their proximity to the 2:1 resonance, while planets c and d appear close to a 5:3 period commensurability, although model degeneracy meant we were unable to retrieve robust TTV masses. Their inflated radii, likely due to extended H-He atmospheres, combined with low insolation makes all three planets excellent candidates for future comparative transmission spectroscopy with JWST.",

keywords = "Planets and satellites: detection, Stars: individual: TOI-2076, Techniques: photometric",

author = "Osborn, \{H. P.\} and A. Bonfanti and D. Gandolfi and C. Hedges and A. Leleu and A. Fortier and D. Futyan and P. Gutermann and Maxted, \{P. F.L.\} and L. Borsato and Collins, \{K. A.\} and \{Da Silva\}, \{J. Gomes\} and Chew, \{Y. Gomez Maqueo\} and Hooton, \{M. J.\} and M. Lendl and H. Parviainen and S. Salmon and N. Schanche and Serrano, \{L. M.\} and Sousa, \{S. G.\} and A. Tuson and S. Ulmer-Moll and \{Van Grootel\}, V. and Wells, \{R. D.\} and Wilson, \{T. G.\} and Y. Alibert and R. Alonso and G. Anglada and J. Asquier and \{Barrado Y Navascues\}, D. and W. Baumjohann and T. Beck and W. Benz and F. Biondi and X. Bonfils and F. Bouchy and A. Brandeker and C. Broeg and T. Barczy and Barros, \{S. C.C.\} and J. Cabrera and S. Charnoz and Cameron, \{A. Collier\} and S. Csizmadia and Davies, \{M. B.\} and M. Deleuil and L. Delrez and Demory, \{B. O.\} and D. Ehrenreich and A. Erikson and L. Fossati and M. Fridlund and M. Gillon and Gomez-Munoz, \{M. A.\} and M. Gudel and K. Heng and S. Hoyer and Isaak, \{K. G.\} and L. Kiss and J. Laskar and \{Des Etangs\}, \{A. Lecavelier\} and C. Lovis and D. Magrin and L. Malavolta and J. McCormac and V. Nascimbeni and G. Olofsson and R. Ottensamer and I. Pagano and E. Palle 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 C. Reimers and I. Ribas and Demangeon, \{O. D.S.\} and Smith, \{A. M.S.\} and L. Sabin and N. Santos and G. Scandariato and U. Schroffenegger and Schwarz, \{R. P.\} and A. Shporer and Simon, \{A. E.\} and M. Steller and Szabo, \{G. M.\} and D. Segransan and N. Thomas and S. Udry and I. Walter and N. Walton",

note = "Funding: ACC and TGW acknowledge support from STFC consolidated grant numbers ST/R000824/1 and ST/V000861/1, and UKSA grant ST/R003203/1.",

year = "2022",

month = aug,

day = "25",

doi = "10.1051/0004-6361/202243065",

language = "English",

volume = "664",

journal = "Astronomy and Astrophysics",

issn = "0004-6361",

publisher = "EDP Sciences",

}

Osborn, HP, Bonfanti, A, Gandolfi, D, Hedges, C, Leleu, A, Fortier, A, Futyan, D, Gutermann, P, Maxted, PFL, Borsato, L, Collins, KA, Da Silva, JG, Chew, YGM, Hooton, MJ, Lendl, M, Parviainen, H, Salmon, S, Schanche, N, Serrano, LM, Sousa, SG, Tuson, A, Ulmer-Moll, S, Van Grootel, V, Wells, RD, Wilson, TG, Alibert, Y, Alonso, R, Anglada, G, Asquier, J, Barrado Y Navascues, D, Baumjohann, W, Beck, T, Benz, W, Biondi, F, Bonfils, X, Bouchy, F, Brandeker, A, Broeg, C, Barczy, T, Barros, SCC, Cabrera, J, Charnoz, S, Cameron, AC, Csizmadia, S, Davies, MB, Deleuil, M, Delrez, L, Demory, BO, Ehrenreich, D, Erikson, A, Fossati, L, Fridlund, M, Gillon, M, Gomez-Munoz, MA, Gudel, M, Heng, K, Hoyer, S, Isaak, KG, Kiss, L, Laskar, J, Des Etangs, AL, Lovis, C, Magrin, D, Malavolta, L, McCormac, J, Nascimbeni, V, Olofsson, G, Ottensamer, R, Pagano, I, Palle, E, Peter, G, Piazza, D, Piotto, G, Pollacco, D, Queloz, D, Ragazzoni, R, Rando, N, Rauer, H, Reimers, C, Ribas, I, Demangeon, ODS, Smith, AMS, Sabin, L, Santos, N, Scandariato, G, Schroffenegger, U, Schwarz, RP, Shporer, A, Simon, AE, Steller, M, Szabo, GM, Segransan, D, Thomas, N, Udry, S, Walter, I & Walton, N 2022, 'Uncovering the true periods of the young sub-Neptunes orbiting TOI-2076', Astronomy and Astrophysics, vol. 664, A156. https://doi.org/10.1051/0004-6361/202243065

TY - JOUR

T1 - Uncovering the true periods of the young sub-Neptunes orbiting TOI-2076

AU - Osborn, H. P.

AU - Bonfanti, A.

AU - Gandolfi, D.

AU - Hedges, C.

AU - Leleu, A.

AU - Fortier, A.

AU - Futyan, D.

AU - Gutermann, P.

AU - Maxted, P. F.L.

AU - Borsato, L.

AU - Collins, K. A.

AU - Da Silva, J. Gomes

AU - Chew, Y. Gomez Maqueo

AU - Hooton, M. J.

AU - Lendl, M.

AU - Parviainen, H.

AU - Salmon, S.

AU - Schanche, N.

AU - Serrano, L. M.

AU - Sousa, S. G.

AU - Tuson, A.

AU - Ulmer-Moll, S.

AU - Van Grootel, V.

AU - Wells, R. D.

AU - Wilson, T. G.

AU - Alibert, Y.

AU - Alonso, R.

AU - Anglada, G.

AU - Asquier, J.

AU - Barrado Y Navascues, D.

AU - Baumjohann, W.

AU - Beck, T.

AU - Benz, W.

AU - Biondi, F.

AU - Bonfils, X.

AU - Bouchy, F.

AU - Brandeker, A.

AU - Broeg, C.

AU - Barczy, T.

AU - Barros, S. C.C.

AU - Cabrera, J.

AU - Charnoz, S.

AU - Cameron, A. Collier

AU - Csizmadia, S.

AU - Davies, M. B.

AU - Deleuil, M.

AU - Delrez, L.

AU - Demory, B. O.

AU - Ehrenreich, D.

AU - Erikson, A.

AU - Fossati, L.

AU - Fridlund, M.

AU - Gillon, M.

AU - Gomez-Munoz, M. A.

AU - Gudel, M.

AU - Heng, K.

AU - Hoyer, S.

AU - Isaak, K. G.

AU - Kiss, L.

AU - Laskar, J.

AU - Des Etangs, A. Lecavelier

AU - Lovis, C.

AU - Magrin, D.

AU - Malavolta, L.

AU - McCormac, J.

AU - Nascimbeni, V.

AU - Olofsson, G.

AU - Ottensamer, R.

AU - Pagano, I.

AU - Palle, 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 - Reimers, C.

AU - Ribas, I.

AU - Demangeon, O. D.S.

AU - Smith, A. M.S.

AU - Sabin, L.

AU - Santos, N.

AU - Scandariato, G.

AU - Schroffenegger, U.

AU - Schwarz, R. P.

AU - Shporer, A.

AU - Simon, A. E.

AU - Steller, M.

AU - Szabo, G. M.

AU - Segransan, D.

AU - Thomas, N.

AU - Udry, S.

AU - Walter, I.

AU - Walton, N.

N1 - Funding: ACC and TGW acknowledge support from STFC consolidated grant numbers ST/R000824/1 and ST/V000861/1, and UKSA grant ST/R003203/1.

PY - 2022/8/25

Y1 - 2022/8/25

N2 - Context. TOI-2076 is a transiting three-planet system of sub-Neptunes orbiting a bright (G = 8.9 mag), young (340 ±80 Myr) K-type star. Although a validated planetary system, the orbits of the two outer planets were unconstrained as only two non-consecutive transits were seen in TESS photometry. This left 11 and 7 possible period aliases for each. Aims. To reveal the true orbits of these two long-period planets, precise photometry targeted on the highest-probability period aliases is required. Long-term monitoring of transits in multi-planet systems can also help constrain planetary masses through TTV measurements. Methods. We used the MonoTools package to determine which aliases to follow, and then performed space-based and ground-based photometric follow-up of TOI-2076 c and d with CHEOPS, SAINT-EX, and LCO telescopes. Results. CHEOPS observations revealed a clear detection for TOI-2076 c at P = 21.01538+0.00084 -0.00074 d, and allowed us to rule out three of the most likely period aliases for TOI-2076 d. Ground-based photometry further enabled us to rule out remaining aliases and confirm the P = 35.12537 ±0.00067 d alias. These observations also improved the radius precision of all three sub-Neptunes to 2.518 ±0.036, 3.497 ±0.043, and 3.232 ±0.063 R⊕. Our observations also revealed a clear anti-correlated TTV signal between planets b and c likely caused by their proximity to the 2:1 resonance, while planets c and d appear close to a 5:3 period commensurability, although model degeneracy meant we were unable to retrieve robust TTV masses. Their inflated radii, likely due to extended H-He atmospheres, combined with low insolation makes all three planets excellent candidates for future comparative transmission spectroscopy with JWST.

AB - Context. TOI-2076 is a transiting three-planet system of sub-Neptunes orbiting a bright (G = 8.9 mag), young (340 ±80 Myr) K-type star. Although a validated planetary system, the orbits of the two outer planets were unconstrained as only two non-consecutive transits were seen in TESS photometry. This left 11 and 7 possible period aliases for each. Aims. To reveal the true orbits of these two long-period planets, precise photometry targeted on the highest-probability period aliases is required. Long-term monitoring of transits in multi-planet systems can also help constrain planetary masses through TTV measurements. Methods. We used the MonoTools package to determine which aliases to follow, and then performed space-based and ground-based photometric follow-up of TOI-2076 c and d with CHEOPS, SAINT-EX, and LCO telescopes. Results. CHEOPS observations revealed a clear detection for TOI-2076 c at P = 21.01538+0.00084 -0.00074 d, and allowed us to rule out three of the most likely period aliases for TOI-2076 d. Ground-based photometry further enabled us to rule out remaining aliases and confirm the P = 35.12537 ±0.00067 d alias. These observations also improved the radius precision of all three sub-Neptunes to 2.518 ±0.036, 3.497 ±0.043, and 3.232 ±0.063 R⊕. Our observations also revealed a clear anti-correlated TTV signal between planets b and c likely caused by their proximity to the 2:1 resonance, while planets c and d appear close to a 5:3 period commensurability, although model degeneracy meant we were unable to retrieve robust TTV masses. Their inflated radii, likely due to extended H-He atmospheres, combined with low insolation makes all three planets excellent candidates for future comparative transmission spectroscopy with JWST.

KW - Planets and satellites: detection

KW - Stars: individual: TOI-2076

KW - Techniques: photometric

UR - https://www.scopus.com/pages/publications/85141293670

U2 - 10.1051/0004-6361/202243065

DO - 10.1051/0004-6361/202243065

M3 - Article

SN - 0004-6361

VL - 664

JO - Astronomy and Astrophysics

JF - Astronomy and Astrophysics

M1 - A156

ER -

Uncovering the true periods of the young sub-Neptunes orbiting TOI-2076

Abstract

Keywords

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Astronomy at St Andrews 2018-2021: Astronomy at St Andrews 2018-2021

Support for the PLATO Development: Support for the PLATO Development Phase 2017-2022: Planet candidate ranking and validation

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Uncovering the true periods of the young sub-Neptunes orbiting TOI-2076

Abstract

Keywords

Access to Document

Other files and links

Fingerprint

Projects

Astronomy at St Andrews 2018-2021: Astronomy at St Andrews 2018-2021

Support for the PLATO Development: Support for the PLATO Development Phase 2017-2022: Planet candidate ranking and validation

Cite this