Dr. Rabus, Markus

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Nombre de publicación
Dr. Rabus, Markus
Nombre completo
Rabus, Markus
Facultad
Email
mrabus@ucsc.cl
ORCID

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2022 - 20232
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Author: Bayliss, D. ×

Research Outputs

Now showing 1 - 2 of 2
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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.
  • Thumbnail Image
    Publication
    HATS-74Ab, HATS-75b, HATS-76b, and HATS-77b: Four Transiting Giant Planets Around K and M Dwarfs
    (The Astronomical Journal, 2022)
    Jordán, Andrés
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    Hartman, J.
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    Bayliss, D.
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    Bakos, G.
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    Brahm, R.
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    Bryant, E.
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    Csubry, Z.
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    Henning, Th.
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    Hobson, M.
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    Mancini, L.
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    Penev, K.
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    Rabus, Markus 
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    Suc, V.
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    Val-Borro, M.
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    Wallace, J.
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    Barkaoui, K.
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    Ciardi, David
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    Collins, K.
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    Esparza Borges, E.
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    Furlan, E.
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    Gan, T.
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    Benkhaldoun, Z.
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    Ghachoui, M.
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    Gillon, M.
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    Howell, S.
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    Jehin, E.
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    Fukui, F.
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    Kawauchi, K.
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    Livingston, J.
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    Luque, R.
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    Matson, R.
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    Matthews, E.
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    Osborn, H.
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    Murgas, F.
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    Narita, Norio
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    Palle, E.
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    Parvianen, H.
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    Waalkes, W.
    The relative rarity of giant planets around low-mass stars compared with solar-type stars is a key prediction from the core-accretion planet formation theory. In this paper we report on the discovery of four gas giant planets that transit low-mass late K and early M dwarfs. The planets HATS-74Ab (TOI 737b), HATS-75b (TOI 552b), HATS-76b (TOI 555b), and HATS-77b (TOI 730b) were all discovered from the HATSouth photometric survey and follow-up using TESS and other photometric facilities. We use the new ESPRESSO facility at the VLT to confirm systems and measure their masses. We find that these planets have masses of 1.46 ± 0.14 MJ, 0.491 ± 0.039 MJ, 2.629 ± 0.089 MJ, and 1.374 0.0740.100-+ MJ, respectively, and radii of 1.032 ± 0.021 RJ, 0.884 ± 0.013 RJ, 1.079 ± 0.031 RJ, and 1.165 ± 0.021 RJ, respectively. The planets all orbit close to their host stars with orbital periods ranging from 1.7319 days to 3.0876 days. With further work, we aim to test core-accretion theory by using these and further discoveries to quantify the occurrence rate of giant planets around low-mass host stars.