Dr. Rabus, Markus

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Dr. Rabus, Markus
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Rabus, Markus
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mrabus@ucsc.cl
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Author: Ballard, S. ×

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    Publication
    A sub-Neptune transiting the young field star HD 18599 at 40 pc
    (Monthly Notices of the Royal Astronomical Society, 2023)
    Dr. Rabus, Markus 
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    De Leon, J.
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    Livingston, J.
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    Jenkins, S.
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    Vines, J.
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    Wittenmyer, R.
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    Clark, J.
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    Winn, J.
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    Addison, B.
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    Ballard, S.
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    Bayliss, D.
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    Beichman, C.
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    Benneke, B.
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    Berardo, D.
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    Bowler, B.
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    Brown, T.
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    Bryant, E.
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    Christiansen, J.
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    Ciardi, D.
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    Collins, K.
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    Collins, K.
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    Crossfield, I.
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    Deming, D.
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    Dragomir, D.
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    Dressing, C.
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    Fukui, A.
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    Gan, T.
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    Giacalone, S.
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    Gill, S.
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    Gorjian, V.
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    Gonzalez-Álvarez, E.
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    Hesse, K.
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    Horner, J.
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    Howell, S.
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    Jenkins, J.
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    Kane, S.
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    Kendall, A.
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    Kielkopf, J.
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    Kreidberg, L.
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    Latham, D.
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    Liu, H.
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    Lund, M.
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    Matson, R.
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    Matthews, E.
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    Mengel, M.
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    Morales, F.
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    Mori, M.
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    Narita, N.
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    Nishiumi, T.
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    Okumura, J.
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    Plavchan, P.
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    Quinn, S.
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    Ricker, G.
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    Rudat, A.
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    Schlieder, J.
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    Schwarz, R.
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    Seager, S.
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    Shporer, A.
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    Smith, A.
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    Stassun, K.
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    Tamura, M.
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    Tan, T.
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    Tinney, C.
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    Vanderspek, R.
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    Werner, M.
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    West, R.
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    Wright, D.
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    Zhang, H.
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    Zhou, G.
    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 2.7 R⊕. The RV data yields a 3-σ mass upper limit of 30.5 M⊕ 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.