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Title: Characterizing 51 Eri b from 1 to 5 μm: A Partly Cloudy Exoplanet

Journal Article · · The Astronomical Journal (Online)
; ;  [1];  [2]; ;  [3];  [4]; ;  [5];  [6];  [7];  [8];  [9];  [10];  [11];  [12];  [13];  [14];  [15];
  1. School of Earth and Space Exploration, Arizona State University, P.O. Box 871404, Tempe, AZ 85287 (United States)
  2. Institut de Recherche sur les Exoplanètes, Départment de Physique, Université de Montréal, Montréal QC H3C 3J7 (Canada)
  3. Astronomy Department, University of California, Berkeley, Berkeley CA 94720 (United States)
  4. NASA Ames Research Center, Mountain View, CA 94035 (United States)
  5. Kavli Institute for Particle Astrophysics and Cosmology, Stanford University, Stanford, CA 94305 (United States)
  6. National Research Council of Canada Herzberg, 5071 West Saanich Rd, Victoria, BC V9E 2E7 (Canada)
  7. Department of Astronomy, Harvard University, Cambridge, MA 02138 (United States)
  8. Space Telescope Science Institute, Baltimore, MD 21218 (United States)
  9. Los Alamos National Laboratory, P.O. Box 1663, MS F663, Los Alamos, NM 87545 (United States)
  10. Lawrence Livermore National Laboratory, Livermore, CA 94551 (United States)
  11. Department of Physics and Astronomy, University of California, Los Angeles, CA 90095 (United States)
  12. Lunar and Planetary Laboratory, University of Arizona, Tucson AZ 85721 (United States)
  13. Subaru Telescope, NAOJ, 650 North A’ohoku Place, Hilo, HI 96720 (United States)
  14. Department of Astrophysical Sciences, Princeton University, Princeton, NJ 08544 (United States)
  15. Dunlap Institute for Astronomy and Astrophysics, University of Toronto, Toronto, ON M5S 3H4 (Canada)
+ Show Author Affiliations

We present spectrophotometry spanning 1–5 μm of 51 Eridani b, a 2–10 M{sub Jup} planet discovered by the Gemini Planet Imager Exoplanet Survey. In this study, we present new K1 (1.90–2.19 μm) and K2 (2.10–2.40 μm) spectra taken with the Gemini Planet Imager as well as an updated L {sub P} (3.76 μm) and new M {sub S} (4.67 μm) photometry from the NIRC2 Narrow camera. The new data were combined with J (1.13–1.35 μm) and H (1.50–1.80 μm) spectra from the discovery epoch with the goal of better characterizing the planet properties. The 51 Eri b photometry is redder than field brown dwarfs as well as known young T-dwarfs with similar spectral type (between T4 and T8), and we propose that 51 Eri b might be in the process of undergoing the transition from L-type to T-type. We used two complementary atmosphere model grids including either deep iron/silicate clouds or sulfide/salt clouds in the photosphere, spanning a range of cloud properties, including fully cloudy, cloud-free, and patchy/intermediate-opacity clouds. The model fits suggest that 51 Eri b has an effective temperature ranging between 605 and 737 K, a solar metallicity, and a surface gravity of log(g) = 3.5–4.0 dex, and the atmosphere requires a patchy cloud atmosphere to model the spectral energy distribution (SED). From the model atmospheres, we infer a luminosity for the planet of −5.83 to −5.93 (logL/L{sub ⊙}), leaving 51 Eri b in the unique position of being one of the only directly imaged planets consistent with having formed via a cold-start scenario. Comparisons of the planet SED against warm-start models indicate that the planet luminosity is best reproduced by a planet formed via core accretion with a core mass between 15 and 127 M{sub ⊕}.

OSTI ID:
22863069
Journal Information:
The Astronomical Journal (Online), Vol. 154, Issue 1; Other Information: Country of input: International Atomic Energy Agency (IAEA); ISSN 1538-3881
Country of Publication:
United States
Language:
English

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79 ASTROPHYSICS
COSMOLOGY AND ASTRONOMY
CLOUDS
COMPARATIVE EVALUATIONS
ENERGY SPECTRA
GRAVITATION
IRON
LUMINOSITY
MASS
METALLICITY
OPACITY
PHOTOMETRY
PHOTOSPHERE
PLANETS
SATELLITE ATMOSPHERES
SATELLITES
SILICATES
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