A Mini-Neptune from TESS and CHEOPS Around the 120 Myr Old AB Dor Member HIP 94235

George Zhou, Christopher P. Wirth, Chelsea X. Huang, Alexander Venner, Kyle Franson, Samuel N. Quinn, L. G. Bouma, Adam L. Kraus, Andrew W. Mann, Elisabeth R. Newton, Diana Dragomir, Alexis Heitzmann, Nataliea Lowson, Stephanie T. Douglas, Matthew Battley, Edward Gillen, Amaury Triaud, David W. Latham, Steve B. Howell, J. D. HartmanBenjamin M. Tofflemire, Robert A. Wittenmyer, Brendan P. Bowler, Jonathan Horner, Stephen R. Kane, John Kielkopf, Peter Plavchan, Duncan J. Wright, Brett C. Addison, Matthew W. Mengel, Jack Okumura, George Ricker, Roland Vanderspek, Sara Seager, Jon M. Jenkins, Joshua N. Winn, Tansu Daylan, Michael Fausnaugh, Michelle Kunimoto

Research output: Contribution to journalArticlepeer-review

Abstract

The Transiting Exoplanet Survey Satellite (TESS) mission has enabled discoveries of the brightest transiting planet systems around young stars. These systems are the benchmarks for testing theories of planetary evolution. We report the discovery of a mini-Neptune transiting a bright star in the AB Doradus moving group. HIP 94235 (TOI-4399, TIC 464646604) is a V mag = 8.31 G-dwarf hosting a 3.00-0.28+0.32R⊠mini-Neptune in a 7.7 day period orbit. HIP 94235 is part of the AB Doradus moving group, one of the youngest and closest associations. Due to its youth, the host star exhibits significant photometric spot modulation, lithium absorption, and X-ray emission. Three 0.06% transits were observed during Sector 27 of the TESS Extended Mission, though these transit signals are dwarfed by the 2% peak-To-peak photometric variability exhibited by the host star. Follow-up observations with the Characterising Exoplanet Satellite confirmed the transit signal and prevented the erosion of the transit ephemeris. HIP 94235 is part of a 50 au G-M binary system. We make use of diffraction limited observations spanning 11 yr, and astrometric accelerations from Hipparcos and Gaia, to constrain the orbit of HIP 94235 B. HIP 94235 is one of the tightest stellar binaries to host an inner planet. As part of a growing sample of bright, young planet systems, HIP 94235 b is ideal for follow-up transit observations, such as those that investigate the evaporative processes driven by high-energy radiation that may sculpt the valleys and deserts in the Neptune population.

Original languageEnglish (US)
Article number289
JournalAstronomical Journal
Volume163
Issue number6
DOIs
StatePublished - Jun 1 2022

All Science Journal Classification (ASJC) codes

  • Astronomy and Astrophysics
  • Space and Planetary Science

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