Journal
ASTRONOMICAL JOURNAL
Volume 153, Issue 4, Pages -Publisher
IOP PUBLISHING LTD
DOI: 10.3847/1538-3881/aa63e9
Keywords
instrumentation: adaptive optics; planetary systems; stars: individual (beta Pictoris); techniques:spectroscopic
Categories
Funding
- Gemini Observatory
- Dunlap Institute, University of Toronto
- NSF Center for Adaptive Optics at UC Santa Cruz
- NSF [AST-0909188, AST-1211562, AST-1405505]
- NASA Origins [NNX11AD21G, NNX10AH31G, NNX14AC21G, NNX15AC89G]
- NASA NExSS [NNX15AD95G]
- University of California Office of the President [LFRP-118057]
- Science and Technology Facilities Council [ST/H002707/1]
- U.S. Department of Energy by Lawrence Livermore National Laboratory [DE-AC52-07NA27344]
- California Institute of Technology/Jet Propulsion Laboratory - NASA through Sagan Fellowship Program
- NASA Exoplanets Research Program (XRP) [NNX16AD44G]
- NASA through Hubble Fellowship - Space Telescope Science Institute [51378.01-A]
- NASA [NAS5-26555]
- NASAs Science Mission Directorate
- NASA [NNX14AC21G, 684457, 133468, NNX10AH31G] Funding Source: Federal RePORTER
- Direct For Mathematical & Physical Scien
- Division Of Astronomical Sciences [1518332, 1411868, 1616097, 1405505] Funding Source: National Science Foundation
- Division Of Astronomical Sciences
- Direct For Mathematical & Physical Scien [1413744, 1615956] Funding Source: National Science Foundation
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Using the Gemini Planet Imager located at Gemini South, we measured the near-infrared (1.0-2.4 mu m) spectrum of the planetary companion to the nearby, young star beta. Pictoris. We compare the spectrum obtained with currently published model grids and with known substellar objects and present the best matching models as well as the best matching observed objects. Comparing the empirical measurement of the bolometric luminosity to evolutionary models, we find a mass of 12.9. +/- 0.2. M-Jup, an effective temperature of 1724. +/- 15 K, a radius of 1.46. +/- 0.01. R-Jup, and a surface gravity of log g = 4.18. 0.01 [dex] (cgs). The stated uncertainties are statistical errors only, and do not incorporate any uncertainty on the evolutionary models. Using atmospheric models, we find an effective temperature of 1700-1800 K and a surface gravity of log g = 3.5-4.0 [dex] depending upon the model. These values agree well with other publications and with hot-start predictions from planetary evolution models. Further, we find that the spectrum of beta Pic. b best matches a low surface gravity L2. +/- 1 brown dwarf. Finally, comparing the spectrum to field brown dwarfs, we find the the spectrum best matches 2MASS J04062677- 381210 and 2MASS J03552337 + 1133437.
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