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An 11 Earth-Mass, Long-Period Sub-Neptune Orbiting a Sun-like Star

Research output: Contribution to journalArticle

  • Andrew W. Mayo
  • Vinesh M. Rajpaul
  • Lars A. Buchhave
  • Courtney D. Dressing
  • Annelies Mortier
  • Li Zeng
  • Charles D. Fortenbach
  • Suzanne Aigrain
  • Aldo S. Bonomo
  • Andrew Collier Cameron
  • David Charbonneau
  • Adrien Coffinet
  • Rosario Cosentino
  • Mario Damasso
  • Xavier Dumusque
  • A. F. Martinez Fiorenzano
  • Raphaëlle D. Haywood
  • David W. Latham
  • Mercedes López-Morales
  • Luca Malavolta
  • Giusi Micela
  • Emilio Molinari
  • Logan Pearce
  • Francesco Pepe
  • David Phillips
  • Giampaolo Piotto
  • Ennio Poretti
  • Alessandro Sozzetti
  • Stephane Udry

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https://iopscience.iop.org/article/10.3847/1538-3881/ab3e2f
Original languageEnglish
Number of pages17
JournalAstronomical Journal
DOIs
Publication statusPublished - 27 Sep 2019

Abstract

Although several thousands of exoplanets have now been detected and characterized, observational biases have led to a paucity of long-period, low-mass exoplanets with measured masses and a corresponding lag in our understanding of such planets. In this paper we report the mass estimation and characterization of the long-period exoplanet Kepler-538b. This planet orbits a Sun-like star (V = 11.27) with M_* = 0.892 +/- (0.051, 0.035) M_sun and R_* = 0.8717 +/- (0.0064, 0.0061) R_sun. Kepler-538b is a 2.215 +/- (0.040, 0.034) R_earth sub-Neptune with a period of P = 81.73778 +/- 0.00013 d. It is the only known planet in the system. We collected radial velocity (RV) observations with HIRES on Keck I and HARPS-N on the TNG. We characterized stellar activity by a Gaussian process with a quasi-periodic kernel applied to our RV and cross correlation function full width at half maximum (FWHM) observations. By simultaneously modeling Kepler photometry, RV, and FWHM observations, we found a semi-amplitude of K = 1.68 +/- (0.39, 0.38) m s^-1 and a planet mass of M_p = 10.6 +/- (2.5, 2.4) M_earth. Kepler-538b is the smallest planet beyond P = 50 d with an RV mass measurement. The planet likely consists of a significant fraction of ices (dominated by water ice), in addition to rocks/metals, and a small amount of gas. Sophisticated modeling techniques such as those used in this paper, combined with future spectrographs with ultra high-precision and stability will be vital for yielding more mass measurements in this poorly understood exoplanet regime. This in turn will improve our understanding of the relationship between planet composition and insolation flux and how the rocky to gaseous transition depends on planetary equilibrium temperature.

    Research areas

  • astro-ph.EP

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