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

Zhou, George and Wirth, Christopher P. and Huang, Chelsea X. 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. and Addison, Brett C. and Mengel, Matthew W. 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 120 Myr Old AB Dor Member HIP 94235. Astronomical Journal, 163 (6). Art. No. 289. ISSN 0004-6256. doi:10.3847/1538-3881/ac69e3. https://resolver.caltech.edu/CaltechAUTHORS:20220608-848590000

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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)^(+0.32) R_⊕ 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.


Item Type:Article
Related URLs:
URLURL TypeDescription
https://doi.org/10.3847/1538-3881/ac69e3DOIArticle
https://arxiv.org/abs/2204.11975arXivDiscussion Paper
ORCID:
AuthorORCID
Zhou, George0000-0002-4891-3517
Wirth, Christopher P.0000-0003-1656-011X
Huang, Chelsea X.0000-0003-0918-7484
Venner, Alexander0000-0002-8400-1646
Franson, Kyle0000-0003-4557-414X
Quinn, Samuel N.0000-0002-8964-8377
Bouma, L. G.0000-0002-0514-5538
Kraus, Adam L.0000-0001-9811-568X
Mann, Andrew W.0000-0003-3654-1602
Newton, Elisabeth. R.0000-0003-4150-841X
Dragomir, Diana0000-0003-2313-467X
Heitzmann, Alexis0000-0002-8091-7526
Lowson, Nataliea0000-0001-6508-5736
Douglas, Stephanie T.0000-0001-7371-2832
Battley, Matthew0000-0002-1357-9774
Gillen, Edward0000-0003-2851-3070
Triaud, Amaury0000-0002-5510-8751
Latham, David W.0000-0001-9911-7388
Howell, Steve B.0000-0002-2532-2853
Hartman, J. D.0000-0001-8732-6166
Tofflemire, Benjamin M.0000-0003-2053-0749
Wittenmyer, Robert A.0000-0001-9957-9304
Bowler, Brendan P.0000-0003-2649-2288
Horner, Jonathan0000-0002-1160-7970
Kane, Stephen R.0000-0002-7084-0529
Kielkopf, John0000-0003-0497-2651
Plavchan, Peter0000-0002-8864-1667
Wright, Duncan J.0000-0001-7294-5386
Addison, Brett C.0000-0003-3216-0626
Mengel, Matthew W.0000-0002-7830-6822
Okumura, Jack0000-0002-4876-8540
Ricker, George0000-0003-2058-6662
Vanderspek, Roland0000-0001-6763-6562
Seager, Sara0000-0002-6892-6948
Jenkins, Jon M.0000-0002-4715-9460
Winn, Joshua N.0000-0002-4265-047X
Daylan, Tansu0000-0002-6939-9211
Fausnaugh, Michael0000-0002-9113-7162
Kunimoto, Michelle0000-0001-9269-8060
Additional Information:© 2022. The Author(s). Published by the American Astronomical Society. Original content from this work may be used under the terms of the Creative Commons Attribution 4.0 licence. Any further distribution of this work must maintain attribution to the author(s) and the title of the work, journal citation and DOI. Received 2022 March 28; revised 2022 April 14; accepted 2022 April 22; published 2022 May 24. We respectfully acknowledge the traditional custodians of all lands throughout Australia, and recognize their continued cultural and spiritual connection to the land, waterways, cosmos, and community. We pay our deepest respects to all Elders, ancestors and descendants of the Giabal, Jarowair, and Kambuwal nations, upon whose lands the MINERVA-Australis facility at Mount Kent is situated. G.Z. thanks the support of the ARC DECRA program DE210101893. C.W. and G.Z. thank the support of the TESS Guest Investigator Program G03007. C.H. thanks the support of the ARC DECRA program DE200101840. E.G. gratefully acknowledges support from the David and Claudia Harding Foundation in the form of a Winton Exoplanet Fellowship. CHEOPS is an ESA mission in partnership with Switzerland with important contributions to the payload and the ground segment from Austria, Belgium, France, Germany, Hungary, Italy, Portugal, Spain, Sweden, and the United Kingdom. We thank support from the CHEOPS GO Programme and Science Operations Centre for help in the preparation and analysis of the CHEOPS observations. This research has used data from the CTIO/SMARTS 1.5 m telescope, which is operated as part of the SMARTS Consortium by RECONS. This study was based in part on observations made using the Las Cumbres Observatory global telescope network, using time allocated by the National Science Foundation's NOIRLab (NOIRLab Prop. ID NOAO2021A-009; principal investigator: J. Hartman). Some of the observations reported in this paper were obtained with the Southern African Large Telescope (SALT). Some of the observations in the paper made use of the high-resolution imaging instrument Zorro obtained under Gemini LLP Proposal Number: GN/S-2021A-LP-105. Zorro was funded by the NASA Exoplanet Exploration Program and built at the NASA Ames Research Center by Steve B. Howell, Nic Scott, Elliott P. Horch, and Emmett Quigley. Zorro was mounted on the Gemini North (and/or South) telescope of the international Gemini Observatory, a program of NSF's OIR Lab, which is managed by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the National Science Foundation on behalf of the Gemini partnership: the National Science Foundation (United States), National Research Council (Canada), Agencia Nacional de Investigación y Desarrollo (Chile), Ministerio de Ciencia, Tecnología e Innovación (Argentina), Ministério da Ciência, Tecnologia, Inovações e Comunicações (Brazil), and Korea Astronomy and Space Science Institute (Republic of Korea). This research has made use of the NASA Exoplanet Archive, which is operated by the California Institute of Technology, under contract with the National Aeronautics and Space Administration under the Exoplanet Exploration Program. Funding for the TESS mission is provided by NASA's Science Mission directorate. 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 made use of the Exoplanet Follow-up Observation Program website, which is operated by the California Institute of Technology, under contract with the National Aeronautics and Space Administration under the Exoplanet Exploration Program. This paper includes data collected by the TESS mission, which are publicly available from the Mikulski Archive for Space Telescopes (MAST). 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. MINERVA-Australis is supported by Australian Research Council LIEF Grant LE160100001, Discovery Grants DP180100972 and DP220100365, Mount Cuba Astronomical Foundation, and institutional partners University of Southern Queensland, UNSW Sydney, MIT, Nanjing University, George Mason University, University of Louisville, University of California Riverside, University of Florida, and The University of Texas at Austin. D.D. acknowledges support from the TESS Guest Investigator Program grants 80NSSC21K0108 and 80NSSC22K0185. Facility: TESS, CHEOPS, Exoplanet Archive, CTIO 1.5 m, LCOGT, Gemini:Zorro, SALT, MINERVA-Australis. Software: emcee (Foreman-Mackey et al. 2013), batman (Kreidberg 2015), astropy (Astropy Collaboration et al. 2018), PyAstronomy (Czesla et al. 2019), comove (Tofflemire et al.2021).
Funders:
Funding AgencyGrant Number
Australian Research CouncilDE210101893
NASAG03007
Australian Research CouncilDE200101840
David and Claudia Harding FoundationUNSPECIFIED
Gemini PartnershipUNSPECIFIED
NASA/JPL/CaltechUNSPECIFIED
Australian Research CouncilLE160100001
Australian Research CouncilDP180100972
Australian Research CouncilDP220100365
Mt. Cuba Astronomical FoundationUNSPECIFIED
NASA80NSSC21K0108
NASA80NSSC22K0185
Subject Keywords:Exoplanet astronomy; Exoplanet evolution; Exoplanet detection methods
Issue or Number:6
Classification Code:Unified Astronomy Thesaurus concepts: Exoplanet astronomy (486); Exoplanet evolution (491); Exoplanet detection methods (489)
DOI:10.3847/1538-3881/ac69e3
Record Number:CaltechAUTHORS:20220608-848590000
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20220608-848590000
Official Citation:George Zhou et al 2022 AJ 163 289
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:115072
Collection:CaltechAUTHORS
Deposited By: George Porter
Deposited On:14 Jun 2022 15:25
Last Modified:14 Jun 2022 15:25

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