Showing papers by "Brian J. Bauman published in 2017"
University of Toronto1, Space Telescope Science Institute2, University of California, Berkeley3, Stanford University4, University of Arizona5, Lawrence Livermore National Laboratory6, University of Western Ontario7, National Institutes of Natural Sciences, Japan8, Princeton University9, University of Georgia10, University of California, Santa Cruz11, Université de Montréal12, University of Victoria13, National Research Council14, University of Grenoble15, University of California, Los Angeles16, Durham University17, University of Michigan18, European Southern Observatory19, Search for extraterrestrial intelligence20, University of California, San Diego21, Ames Research Center22, California Institute of Technology23, American Museum of Natural History24, Arizona State University25, Universities Space Research Association26, Cornell University27, The Aerospace Corporation28, Johns Hopkins University29
TL;DR: Gemini Observatory, Dunlap Institute, University of Toronto, NSF Center for Adaptive Optics at UC Santa Cruz; NSF [AST-0909188], AST-1211562, AST-1405505] as mentioned in this paper.
Abstract: 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
97 citations
University of Toronto1, Space Telescope Science Institute2, University of California, Berkeley3, Stanford University4, University of Arizona5, Lawrence Livermore National Laboratory6, University of Western Ontario7, Subaru8, Princeton University9, University of Georgia10, University of California, Santa Cruz11, Université de Montréal12, National Research Council13, University of California, Los Angeles14, University of Michigan15, European Southern Observatory16, University of California, San Diego17, Search for extraterrestrial intelligence18, Ames Research Center19, American Museum of Natural History20, Arizona State University21, Universities Space Research Association22, Cornell University23, California Institute of Technology24, The Aerospace Corporation25, Johns Hopkins University26
TL;DR: In this paper, the Gemini Planet Imager (GPI) was used to measure the near-infrared (1.0-2.4 micron) spectrum of the planetary companion to the nearby, young star Pictoris.
Abstract: Using the Gemini Planet Imager (GPI) located at Gemini South, we measured the near-infrared (1.0-2.4 micron) 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 $12.9\pm0.2$ $\mathcal{M}_\mathrm{Jup}$, an effective temperature of $1724\pm15$ K, a radius of $1.46\pm0.01$ $\mathcal{R}_\mathrm{Jup}$, and a surface gravity of $\log g = 4.18\pm0.01$ [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 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$\pm$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.
74 citations