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

Zhou, George ORCID: https://orcid.org/0000-0002-4891-3517 and Wirth, Christopher P. and Huang, Chelsea X. ORCID: https://orcid.org/0000-0003-0918-7484 and Venner, Alexander and Franson, Kyle and Quinn, Samuel N. and Bouma, L. G. and Kraus, Adam L. and Mann, Andrew W. and Newton, Elisabeth. R. and Dragomir, Diana and Heitzmann, Alexis and Lowson, Nataliea and Douglas, Stephanie T. and Battley, Matthew and Gillen, Edward and Triaud, Amaury and Latham, David W. and Howell, Steve B. and Hartman, J. D. and Tofflemire, Benjamin M. and Wittenmyer, Robert A. and Bowler, Brendan P. and Horner, Jonathan and Kane, Stephen R. and Kielkopf, John and Plavchan, Peter and Wright, Duncan J. ORCID: https://orcid.org/0000-0001-7294-5386 and Addison, Brett C. ORCID: https://orcid.org/0000-0003-3216-0626 and Mengel, Matthew W. ORCID: https://orcid.org/0000-0002-7830-6822 and Okumura, Jack and Ricker, George and Vanderspek, Roland and Seager, Sara and Jenkins, Jon M. and Winn, Joshua N. and Daylan, Tansu and Fausnaugh, Michael and Kunimoto, Michelle (2022) A Mini-Neptune from TESS and CHEOPS Around the 120Myr Old AB Dor Member HIP 94235. The Astronomical Journal, 163 (6):289. pp. 1-19. ISSN 0004-6256

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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.


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Item Type: Article (Commonwealth Reporting Category C)
Refereed: Yes
Item Status: Live Archive
Faculty/School / Institute/Centre: Current - Institute for Advanced Engineering and Space Sciences - Centre for Astrophysics (1 Aug 2018 -)
Faculty/School / Institute/Centre: Current - Institute for Advanced Engineering and Space Sciences - Centre for Astrophysics (1 Aug 2018 -)
Date Deposited: 18 Jul 2022 02:02
Last Modified: 17 Oct 2022 00:42
Uncontrolled Keywords: Exoplanet astronomy; Exoplanet evolution; Exoplanet detection; methods; Astrophysics - Earth and Planetary Astrophysics; Astrophysics - Solar and Stellar Astrophysics
Fields of Research (2020): 51 PHYSICAL SCIENCES > 5101 Astronomical sciences > 510109 Stellar astronomy and planetary systems
Socio-Economic Objectives (2020): 28 EXPANDING KNOWLEDGE > 2801 Expanding knowledge > 280120 Expanding knowledge in the physical sciences
Identification Number or DOI: https://doi.org/10.3847/1538-3881/ac69e3
URI: http://eprints.usq.edu.au/id/eprint/49476

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