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

Emil Knudstrup, Luisa M. Serrano, Davide Gandolfi, Simon H. Albrecht, William D. Cochran, Michael Endl, Phillip MacQueen, René Tronsgaard, Allyson Bieryla, Lars A. Buchhave, Keivan Stassun, Karen A. Collins, Grzegorz Nowak, Hans J. Deeg, Khalid Barkaoui, Boris S. Safonov, Ivan A. Strakhov, Alexandre A. Belinski, Joseph D. Twicken, Jon M. JenkinsAndrew W. Howard, Howard Isaacson, Joshua N. Winn, Kevin Collins, Dennis M. Conti, Gabor Furesz, Tianjun Gan, John F. Kielkopf, Bob Massey, Felipe Murgas, Lauren G. Murphy, Enric Palle, Samuel N. Quinn, Phillip A. Reed, George R. Ricker, Sara Seager, Bernie Shiao, Richard P. Schwarz, Gregor Srdoc, David Watanabe

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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 shortperiod 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)(+33)degrees. As these planets are all found in relatively bright systems (V similar to 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.
Original languageEnglish
Article numberA22
JournalAstronomy and Astrophysics
Number of pages18
Publication statusPublished - 2022


  • Planets and satellites: detection
  • Planets and satellites: gaseous planets
  • Planet-star interactions
  • Techniques: radial velocities
  • Techniques: photometric


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