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Published January 1, 2020 | Version v1
Journal article Open

The CARMENES search for exoplanets around M dwarfs: LP 714-47 b (TOI 442.01): populating the Neptune desert

Creators

  • 1. Georg August Univ, Inst Astrophys, Friedrich Hund Pl 1, D-37077 Gottingen, Germany
  • 2. Univ Kansas, Dept Phys & Astron, Lawrence, KS 66045 USA
  • 3. Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany
  • 4. George Mason Univ, Dept Phys & Astron, 4400 Univ Dr MS 3F3, Fairfax, VA 22030 USA
  • 5. Heidelberg Univ, Landessternwarte, Zentrum Astron, Konigstuhl 12, D-69117 Heidelberg, Germany
  • 6. Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA
  • 7. Vanderbilt Univ, Phys & Astron Dept, 6301 Stevenson Ctr Ln, Nashville, TN 37235 USA
  • 8. ESAC, Ctr Astrobiol CSIC INTA, Camino Bajo del Castillo S-N, Madrid 28692, Spain
  • 9. Cadi Ayyad Univ, Oukaimeden Observ, High Energy Phys & Astrophys Lab, Marrakech, Morocco

Description

We report the discovery of a Neptune-like planet (LP 714-47 b, P = 4.05204 d, m(b) = 30.8 +/- 1.5M(circle plus), R-b = 4.7 +/- 0.3 R-circle plus) located in the "hot Neptune desert". Confirmation of the TESS Object of Interest (TOI 442.01) was achieved with radial-velocity follow-up using CARMENES, ESPRESSO, HIRES, iSHELL, and PFS, as well as from photometric data using TESS, Spitzer, and ground-based photometry from MuSCAT2, TRAPPIST-South, MONET-South, the George Mason University telescope, the Las Cumbres Observatory Global Telescope network, the El Sauce telescope, the TuBTAK National Observatory, the University of Louisville Manner Telescope, and WASP-South. We also present high-spatial resolution adaptive optics imaging with the Gemini Near-Infrared Imager. The low uncertainties in the mass and radius determination place LP 714-47 b among physically well-characterised planets, allowing for a meaningful comparison with planet structure models. The host star LP 714-47 is a slowly rotating early M dwarf (T-eff = 3950 +/- 51 K) with a mass of 0.59 +/- 0.02M(circle dot) and a radius of 0.58 +/- 0.02R(circle dot). From long-term photometric monitoring and spectroscopic activity indicators, we determine a stellar rotation period of about 33 d. The stellar activity is also manifested as correlated noise in the radial-velocity data. In the power spectrum of the radial-velocity data, we detect a second signal with a period of 16 days in addition to the four-day signal of the planet. This could be shown to be a harmonic of the stellar rotation period or the signal of a second planet. It may be possible to tell the difference once more TESS data and radial-velocity data are obtained.

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