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Confirmation and characterisation of three giant planets detected by TESS from the FIES/NOT and Tull/McDonald spectrographs

Knudstrup, Emil and Serrano, Luisa M. and Gandolfi, Davide and Albrecht, Simon H. and Cochran, William D. and Endl, Michael and MacQueen, Phillip and Tronsgaard, René and Bieryla, Allyson and Buchhave, Lars A. and Stassun, Keivan and Collins, Karen A. and Nowak, Grzegorz and Deeg, Hans J. and Barkaoui, Khalid and Safonov, Boris S. and Strakhov, Ivan A. and Belinski, Alexandre A. and Twicken, Joseph D. and Jenkins, Jon M. and Howard, Andrew W. and Isaacson, Howard and Winn, Joshua N. and Collins, Kevin I. and Conti, Dennis M. and Furesz, Gabor and Gan, Tianjun and Kielkopf, John F. and Massey, Bob and Murgas, Felipe and Murphy, Lauren G. and Palle, Enric and Quinn, Samuel N. and Reed, Phillip A. and Ricker, George R. and Seager, Sara and Shiao, Bernie and Schwarz, Richard P. and Srdoc, Gregor and Watanabe, David (2022) Confirmation and characterisation of three giant planets detected by TESS from the FIES/NOT and Tull/McDonald spectrographs. Astronomy and Astrophysics, 667 . Art. No. A22. ISSN 0004-6361. doi:10.1051/0004-6361/202243656.

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We report the confirmation and characterisation of TOI-1820 b, TOI-2025 b, and TOI-2158 b, three Jupiter-sized planets on short-period orbits around G-type stars detected by TESS. Through our ground-based efforts using the FIES and Tull spectrographs, we have confirmed these planets and characterised their orbits, and find periods of around 4.9 d, 8.9 d, and 8.6 d for TOI-1820 b, TOI-2025 b, and TOI-2158 b, respectively. The sizes of the planets range from 0.96 to 1.14 Jupiter radii, and their masses are in the range from 0.8 to 4.4 Jupiter masses. For two of the systems, namely TOI-2025 and TOI-2158, we see a long-term trend in the radial velocities, indicating the presence of an outer companion in each of the two systems. For TOI-2025 we furthermore find the star to be well aligned with the orbit, with a projected obliquity of 9_(−31)^(+33ₒ). As these planets are all found in relatively bright systems (V ~ 10.9–11.6 mag), they are well suited for further studies, which could help shed light on the formation and migration of hot and warm Jupiters.

Item Type:Article
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URLURL TypeDescription
Knudstrup, Emil0000-0001-7880-594X
Serrano, Luisa M.0000-0001-9211-3691
Gandolfi, Davide0000-0001-8627-9628
Albrecht, Simon H.0000-0002-5960-6803
Cochran, William D.0000-0001-9662-3496
Endl, Michael0000-0002-7714-6310
Tronsgaard, René0000-0003-1001-0707
Bieryla, Allyson0000-0001-6637-5401
Buchhave, Lars A.0000-0003-1605-5666
Stassun, Keivan0000-0002-3481-9052
Collins, Karen A.0000-0001-6588-9574
Nowak, Grzegorz0000-0002-7031-7754
Deeg, Hans J.0000-0003-0047-4241
Barkaoui, Khalid0000-0003-1464-9276
Safonov, Boris S.0000-0003-1713-3208
Strakhov, Ivan A.0000-0003-0647-6133
Belinski, Alexandre A.0000-0003-3469-0989
Twicken, Joseph D.0000-0002-6778-7552
Jenkins, Jon M.0000-0002-4715-9460
Howard, Andrew W.0000-0001-8638-0320
Isaacson, Howard0000-0002-0531-1073
Winn, Joshua N.0000-0002-4265-047X
Collins, Kevin I.0000-0003-2781-3207
Conti, Dennis M.0000-0003-2239-0567
Gan, Tianjun0000-0002-4503-9705
Kielkopf, John F.0000-0003-0497-2651
Massey, Bob0000-0001-8879-7138
Murgas, Felipe0000-0001-9087-1245
Murphy, Lauren G.0000-0003-3796-6303
Palle, Enric0000-0003-0987-1593
Quinn, Samuel N.0000-0002-8964-8377
Reed, Phillip A.0000-0002-5005-1215
Ricker, George R.0000-0003-2058-6662
Seager, Sara0000-0002-6892-6948
Shiao, Bernie0000-0001-7842-3714
Schwarz, Richard P.0000-0001-8227-1020
Watanabe, David0000-0002-3555-8464
Additional Information:The authors would like to thank the referee, Louise D. Nielsen, for an insightful and helpful review of this work. The authors would also like to thank the staff at the Nordic Optical Telescope for their help and expertise. This paper includes data taken at the Nordic Optical Telescope under the programs IDs 59-210, 59-503, 61-510, 61-804, 62-506, and 63-505. This study is based on observations made with the Nordic Optical Telescope, owned in collaboration by the University of Turku and Aarhus University, and operated jointly by Aarhus University, the University of Turku and the University of Oslo, representing Denmark, Finland, and Norway, the University of Iceland and Stockholm University at the Observatorio del Roque de los Muchachos, La Palma, Spain, of the Instituto de Astrofísica de Canarias. This paper includes data taken at The McDonald Observatory of The University of Texas at Austin. This is University of Texas Center for Planetary Systems Habitability contribution #0053. We acknowledge the use of public TESS data from pipelines at the TESS Science Office and at the TESS Science Processing Operations Center. Resources supporting this work were provided by the NASA High-End Computing (HEC) programme through the NASA Advanced Supercomputing (NAS) Division at Ames Research Center for the production of the SPOC data products. Funding for the Stellar Astrophysics Centre is provided by The Danish National Research Foundation (Grant agreement no.: DNRF106). A.A.B., B.S.S., and I.A.S. acknowledge the support of Ministry of Science and Higher Education of the Russian Federation under the grant 075-15-2020-780(N13.1902.21.0039). The numerical results presented in this work were obtained at the Centre for Scientific Computing, Aarhus This work makes use of observations from the LCOGT network. Part of the LCOGT telescope time was granted by NOIRLab through the Mid-Scale Innovations Program (MSIP). MSIP is funded by NSF. P.R. and L.M. acknowledge support from National Science Foundation grant No. 1952545. This research made use of Astropy ( a community-developed core Python package for Astronomy (Astropy Collaboration 2013, 2018). This researchmade use of matplotlib (Hunter 2007). This research made use of TESScut (Brasseur et al. 2019). This research made use of astroplan (Morris et al. 2018). This research made use of SciPy (Virtanen et al. 2020). This research made use of corner (Foreman-Mackey 2016).
Group:Astronomy Department
Funding AgencyGrant Number
Danish National Research FoundationDNRF106
Record Number:CaltechAUTHORS:20221122-564647900.22
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Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:118005
Deposited By: Research Services Depository
Deposited On:06 Dec 2022 00:51
Last Modified:06 Dec 2022 17:21

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