Journal
ASTRONOMY & ASTROPHYSICS
Volume 664, Issue -, Pages -Publisher
EDP SCIENCES S A
DOI: 10.1051/0004-6361/202243065
Keywords
planets and satellites: detection; stars: individual: TOI-2076; techniques: photometric
Categories
Funding
- National Science Foundation through the US Community [2034337]
- JSPS KAKENHI [JP18H05439]
- JST PRESTO [JPMJPR1775]
- NSF
- STFC PhD studentship
- Swiss National Science Foundation
- Cassa di Risparmio di Torino (CRT) foundation [2018.2323]
- FCT [CEECIND/00826/2018, 57/2016/CP1364/CT0004]
- FCT -Fundaccao para a Ciencia e Tecnologia
- FEDER through COMPETE2020 -Programa Operacional Competitividade e Internacionalizacao [PTDC/FIS-AST/32113/2017, POCI-01-0145-FEDER-032113, PTDC/FIS-AST/28953/2017, POCI-01-0145-FEDER-028953, PTDC/FISAST/28987/2017, POCI-01-0145-FEDER-028987]
- STFC [ST/R000824/1, ST/V000861/1, ST/M001040/1]
- UKSA [ST/R003203/1]
- Belgian Federal Science Policy Office (BELSPO)
- University of Liege through an ARC grant for Concerted Research Actions - Wallonia-Brussels Federation
- Italian Space Agency (ASI) [2013-016-R.0]
- Swiss National Fund [200020_172746]
- Swiss National Science Foundation [PCEFP2_194576, PP00P2-190080, 200021_200726]
- SNSA
- Spanish Ministry of Economics and Competitiveness [PGC2018-098153-B-C31]
- Spanish Ministry of Science and Innovation and the European Regional Development Fund [PGC2018098153-B-C33]
- Generalitat de Catalunya/CERCA programme
- Hungarian National Research, Development and Innovation Office (NKFIH) [K-125015]
- PRODEX Experiment Agreement [4000137122]
- Lendulet grant of the Hungarian Academy of Science [LP2018-7/2021]
- city of Szombathely
- project Equip@Meso of the programme Investissements d'Avenir [ANR-10-EQPX-29-01]
- Swedish National Space Agency [65/19, 174/18]
- European Regional Development Fund [PGC2018-098153-B-C31, ESP2016-80435-C2-1-R, ESP2016-80435-C2-2-R, PGC2018-098153-B-C33, ESP2017-87676-C5-1R, MDM-2017-0737]
- ESA [4000124370]
- European Research Council (ERC) under the European Union's Horizon 2020 research and innovation programme (project FOUR ACES) [724427]
- Simons Foundation [327127]
- CNES [837319]
- European Research Council (ERC) under the European Unions Horizon 2020 research and innovation programme [833925]
- [UNAM-PAPIIT-IG101321]
- Direct For Mathematical & Physical Scien
- Division Of Astronomical Sciences [2034337] Funding Source: National Science Foundation
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This study reveals the true orbits of the two long-period planets in the TOI-2076 system through precise photometry. The observations also suggest that these three planets have inflated radii and low insolation, making them excellent candidates for future comparative transmission spectroscopy with JWST.
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(-0.00074)(+0.00084) 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-circle plus. 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.
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