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Yayınlanmış 1 Ocak 2021 | Sürüm v1
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Discovery of a young low-mass brown dwarf transiting a fast-rotating F-type star by the Galactic Plane eXoplanet (GPX) survey

Oluşturanlar

  • 1. Acton Sky Portal Private Observ, Acton, MA 01720 USA
  • 2. Ural Fed Univ, Lab Astrochem Res, Mira St 19, Ekaterinburg 620002, Russia
  • 3. Univ Grenoble Alpes, IPAG, CNRS, F-38000 Grenoble, France
  • 4. Univ Paris 06, Inst Astrophys Paris, UMR7095 CNRS, 98bis Blvd Arago, F-75014 Paris, France
  • 5. Univ Porto, Inst Astrofis & Ciencias Espaco, CAUP, Rua Estrelas, P-4150762 Porto, Portugal
  • 6. INAF Osservatorio Astrofis Arcetri, Largo E Fermi 5, I-50125 Florence, Italy
  • 7. Lehigh Univ, Dept Phys, 16 Mem Dr East, Bethlehem, PA 18015 USA
  • 8. Vanderbilt Univ, Dept Phys & Astron, 6301 Stevenson Ctr Ln, Nashville, TN 37235 USA
  • 9. Univ Texas Austin, Dept Astron, Austin, TX 78712 USA
  • 10. Moscow MV Lomonosov State Univ, Sternberg Astron Inst, 13 Univ Skij Pr, Moscow 119234, Russia
  • 11. Moscow MV Lomonosov State Univ, Fac Phys, Leninskie Gory 1, Moscow 119991, Russia
  • 12. Natl Youth Space Ctr, Goheung 59567, Jeollanam Do, South Korea
  • 13. RAS, Fed State Budget Sci Inst Crimean Astrophys Obser, Nauchny 298409, Crimea, Russia
  • 14. Russian Acad Sci, Special Astrophys Observ, Nizhnii Arkhyz 369167, Russia

Açıklama

We announce the discovery of GPX-1 b, a transiting brown dwarf with a mass of 19.7 +/- 1.6 M-Jup and a radius of 1.47 +/- 0.10 R-Jup, the first substellar object discovered by the Galactic Plane eXoplanet (GPX) survey. The brown dwarf transits a moderately bright (V = 12.3 mag) fast-rotating F-type star with a projected rotational velocity v sin i(*) = 40 +/- 10 km s(-1). We use the isochrone placement algorithm to characterize the host star, which has effective temperature 7000 +/- 200 K, mass 1.68 +/- 0.10 M-circle dot, radius 1.56 +/- 0.10 R-circle dot, and approximate age 0.27(-0.15)(+0.09) Gyr. GPX-1 b has an orbital period of similar to 1.75 d and a transit depth of 0.90 +/- 0.03 per cent. We describe the GPX transit detection observations, subsequent photometric and speckle-interferometric follow-up observations, and SOPHIE spectroscopic measurements, which allowed us to establish the presence of a substellar object around the host star. GPX-1 was observed at 30-min integrations by TESS in Sector 18, but the data are affected by blending with a 3.4 mag brighter star 42 arcsec away. GPX-1 b is one of about two dozen transiting brown dwarfs known to date, with a mass close to the theoretical brown dwarf/gas giant planet mass transition boundary. Since GPX-1 is a moderately bright and fast-rotating star, it can be followed-up by the means of the Doppler tomography.

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