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  • A sub-Neptune transiting the young field star HD 18599 at 40 pc
    de Leon, Jerome P; Livingston, John H; Jenkins, James S; Vines, Jose I; Wittenmyer, Robert A; Clark, Jake T; Winn, Joshua I M; Addison, Brett; Ballard, Sarah; Bayliss, Daniel; Beichman, Charles; Benneke, Björn; Berardo, David Anthony; Bowler, Brendan P; Brown, Tim; Bryant, Edward M; Christiansen, Jessie; Ciardi, David; Collins, Karen A; Collins, Kevin I; Crossfield, Ian; Drake Deming; Dragomir, Diana; Dressing, Courtney D; Fukui, Akihiko; Gan, Tianjun; Giacalone, Steven; Gill, Samuel; Erica Gonz\' alez Alvarez; Hesse, Katharine; Horner, Jonathan; Howell, Steve B; Jenkins, Jon M; Kane, Stephen R; Kendall, Alicia; Kielkopf, John F; Kreidberg, Laura; Latham, David W; Liu, Huigen; Lund, Michael B; Matson, Rachel; Matthews, Elisabeth; Mengel, Matthew W; Morales, Farisa; Mori, Mayuko; Narita, Norio; Nishiumi, Taku; Okumura, Jack; Plavchan, Peter; Quinn, Sam; Rabus, Markus; Ricker, George; Rudat, Alexander; Schlieder, Joshua; Schwarz, Richard P; Seager, Sara; Shporer, Avi; Smith, Alexis M S; Sphorer, Avi; Stassun, Keivan; Tamura, Motohide; Thiam Guan Tan; Tinney, C G; Vanderspek, Roland; Gorjian, Varoujan; Werner, Michael W; West, Richard G; Wright, Duncan; Zhang, Hui; Zhou, George

    arXiv (Cornell University), 10/2022
    Paper, Journal Article

    Transiting exoplanets orbiting young nearby stars are ideal laboratories for testing theories of planet formation and evolution. However, to date only a handful of stars with age <1 Gyr have been found to host transiting exoplanets. Here we present the discovery and validation of a sub-Neptune around HD 18599, a young (300 Myr), nearby (d=40 pc) K star. We validate the transiting planet candidate as a bona fide planet using data from the TESS, Spitzer, and Gaia missions, ground-based photometry from IRSF, LCO, PEST, and NGTS, speckle imaging from Gemini, and spectroscopy from CHIRON, NRES, FEROS, and Minerva-Australis. The planet has an orbital period of 4.13 d, and a radius of 2.7Rearth. The RV data yields a 3-sigma mass upper limit of 30.5Mearth which is explained by either a massive companion or the large observed jitter typical for a young star. The brightness of the host star (V~9 mag) makes it conducive to detailed characterization via Doppler mass measurement which will provide a rare view into the interior structure of young planets.

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