Otegi, J. F. and Bouchy, F. and Helled, R. and Armstrong, D. J. and Stalport, M. and Psaridi, A. and Delisle, J.-B. and Stassun, K.G. and Delgado-Mena, E. and Santos, N. C. and Hara, N. C. and Collins, K. and Gandhi, S. and Dorn, C. and Brogi, M. and Fridlund, M. and Osborn, H. P. and Hoyer, S. and Udry, S. and Hojjatpanah, S. and Nielsen, L. D. and Dumusque, X. and Adibekyan, V. and Conti, D. and Schwarz, R. and Wang, G. and Figueira, P. and Lillo-Box, J. and Hadjigeorghiou, A. and Bayliss, D. and Strøm, P. A. and Sousa, S. G. and Barrado, D. and Osborn, A. and Barros, S. C. C. and Brown, D. J. A. and Eastman, J. D. and Ciardi, D. R. and Vanderburg, A. and Goeke, R. F. and Guerrero, N. M. and Boyd, P. T. and Caldwell, D. A. and Henze, C. E. and McLean, B. and Ricker, G. and Vanderspek, R. and Latham, D. W. and Seager, S. and Winn, J. and Jenkins, J. M. (2021) TESS and HARPS reveal two sub-Neptunes around TOI 1062. Astronomy and Astrophysics, 653 . Art. No. A105. ISSN 0004-6361. doi:10.1051/0004-6361/202040247. https://resolver.caltech.edu/CaltechAUTHORS:20211011-161351659
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Abstract
The Transiting Exoplanet Survey Satellite (TESS) mission was designed to perform an all-sky search of planets around bright and nearby stars. Here we report the discovery of two sub-Neptunes orbiting around TOI 1062 (TIC 299799658), a V = 10.25 G9V star observed in the TESS Sectors 1, 13, 27, and 28. We use precise radial velocity observations from HARPS to confirm and characterize these two planets. TOI 1062b has a radius of 2.265_(−0.091)^(+0.096) R_⊕, a mass of 10.15 ± 0.8 M_⊕, and an orbital period of 4.1130 ± 0.0015 days. The second planet is not transiting, has a minimum mass of 9.78−1.18+1.26 M_⊕ and is near the 2:1 mean motion resonance with the innermost planet with an orbital period of 7.972_(−0.024)^(+0.018) days. We performed a dynamical analysis to explore the proximity of the system to this resonance, and to attempt further constraining the orbital parameters. The transiting planet has a mean density of 4.85_(−0.74)^(+0.84_ g cm⁻³ and an analysis of its internal structure reveals that it is expected to have a small volatile envelope accounting for 0.35% of the mass at most. The star’s brightness and the proximity of the inner planet to what is know as the radius gap make it an interesting candidate for transmission spectroscopy, which could further constrain the composition and internal structure of TOI 1062b.
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| Additional Information: | © ESO 2021. Article published by EDP Sciences. Received 27 December 2020; Accepted 5 May 2021; Published online 15 September 2021. This work has been in particular carried out in the frame of the National Centre for Competence in Research ‘PlanetS’ supported by SNSF. D.J.A. acknowledges support from the STFC via an Ernest Rutherford Fellowship (ST/R00384X/1). This work was supported by FCT - Fundação para a Ciência e a Tecnologia through national funds and by FEDER through COMPETE2020 - Programa Operacional Competitividade e Internacionalização by these grants: UID/FIS/04434/2019; UIDB/04434/2020; UIDP/04434/2020; PTDC/FIS-AST/32113/2017 and POCI-01-0145-FEDER-032113; PTDC/FIS-AST/28953/2017 and POCI-01-0145-FEDER-028953. V.A. and E.D.M acknowledge the support from FCT through InvestigadorFCT contracts nr. IF/00650/2015/CP1273/CT0001, IF/00849/2015/CP1273/CT0003, respectively. C.D. acknowledges support from the Swiss National Science Foundation under grant PZ00P2_174028. Siddharth Gandhi acknowledges support from the UK Science and Technology Facilities Council (STFC) research grant ST/S000631/1. Resources supporting this work were provided by the NASA High-End Computing (HEC) Program through the NASA Advanced Supercomputing (NAS) Division at Ames Research Center for the production of the SPOC data products. We acknowledge the use of public TESS Alert data from pipelines at the TESS Science Office and at the TESS Science Processing Operations Center. This research has been partly funded by the Spanish State Research Agency (AEI) Projects No. ESP2017-87676-C5-1-R and No. MDM-2017-0737 Unidad de Excelencia “María de Maeztu”- Centro de Astrobiología (INTA-CSIC). S.G.S acknowledges the support from FCT through Investigador FCT contract nr. CEECIND/00826/2018 and POPH/FSE (EC). H.P.O. acknowledges that this work has been carried out within the framework of the NCCR PlanetS supported by the Swiss National Science Foundation. S.H. acknowledges support by the fellowships PD/BD/128119/2016 funded by FCT (Portugal). X.D is grateful to The Branco Weiss Fellowship–Society in Science for its financial support. This project has received funding from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme (grant agreement No 851555/SCORE. A.O acknowledges support from an STFC studentship. S.H acknowledges CNES funding through the grant 837319.This work was supported by FCT through national funds (PTDC/FIS-AST/28953/2017) and by FEDER - Fundo Europeu de Desenvolvimento Regional through COMPETE2020 - Programa Operacional Competitividade e Internacionalização (POCI-01-0145-FEDER-028953) and through national funds (PIDDAC) by the grant UID/FIS/04434/2019. Funding for the TESS mission is provided by NASA’s Science Mission directorate. This work makes use of observations from the LCOGT network. | ||||||||||||||||||||||||||||||||||||||||||||||||||
| Group: | Infrared Processing and Analysis Center (IPAC) | ||||||||||||||||||||||||||||||||||||||||||||||||||
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| Subject Keywords: | planets and satellites: general – planets and satellites: detection – planets and satellites: composition | ||||||||||||||||||||||||||||||||||||||||||||||||||
| DOI: | 10.1051/0004-6361/202040247 | ||||||||||||||||||||||||||||||||||||||||||||||||||
| Record Number: | CaltechAUTHORS:20211011-161351659 | ||||||||||||||||||||||||||||||||||||||||||||||||||
| Persistent URL: | https://resolver.caltech.edu/CaltechAUTHORS:20211011-161351659 | ||||||||||||||||||||||||||||||||||||||||||||||||||
| Official Citation: | TESS and HARPS reveal two sub-Neptunes around TOI 1062. J. F. Otegi, F. Bouchy, R. Helled, D. J. Armstrong, M. Stalport, A. Psaridi, J.-B. Delisle, K.G. Stassun, E. Delgado-Mena, N. C. Santos, N. C. Hara, K. Collins, S. Gandhi, C. Dorn, M. Brogi, M. Fridlund, H. P. Osborn, S. Hoyer, S. Udry, S. Hojjatpanah, L. D. Nielsen, X. Dumusque, V. Adibekyan, D. Conti, R. Schwarz, G. Wang, P. Figueira, J. Lillo-Box, A. Hadjigeorghiou, D. Bayliss, P. A. Strøm, S. G. Sousa, D. Barrado, A. Osborn, S. C. C. Barros, D. J. A. Brown, J. D. Eastman, D. R. Ciardi, A. Vanderburg, R. F. Goeke, N. M. Guerrero, P. T. Boyd, D. A. Caldwell, C. E. Henze, B. McLean, G. Ricker, R. Vanderspek, D. W. Latham, S. Seager, J. Winn and J. M. Jenkins. A&A, 653 (2021) A105; DOI: https://doi.org/10.1051/0004-6361/202040247 | ||||||||||||||||||||||||||||||||||||||||||||||||||
| Usage Policy: | No commercial reproduction, distribution, display or performance rights in this work are provided. | ||||||||||||||||||||||||||||||||||||||||||||||||||
| ID Code: | 111349 | ||||||||||||||||||||||||||||||||||||||||||||||||||
| Collection: | CaltechAUTHORS | ||||||||||||||||||||||||||||||||||||||||||||||||||
| Deposited By: | Tony Diaz | ||||||||||||||||||||||||||||||||||||||||||||||||||
| Deposited On: | 11 Oct 2021 17:48 | ||||||||||||||||||||||||||||||||||||||||||||||||||
| Last Modified: | 11 Oct 2021 17:48 |
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