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1–2.4 μm near-IR spectrum of the giant planet β Pictoris b obtained with the Gemini Planet Imager.

Chilcote, Jeffrey and Pueyo, Laurent and De Rosa, Robert J. and Vargas, Jeffrey and Macintosh, Bruce and Bailey, Vanessa P. and Barman, Travis and Bauman, Brian and Bruzzone, Sebastian and Bulger, Joanna and Burrows, Adam S. and Cardwell, Andrew and Chen, Christine H. and Cotten, Tara and Dillon, Daren and Doyon, Rene and Draper, Zachary H. and Duchêne, Gaspard and Dunn, Jennifer and Erikson, Darren and Fitzgerald, Michael P. and Follette, Katherine B. and Gavel, Donald and Goodsell, Stephen J. and Graham, James R. and Greenbaum, Alexandra Z. and Hartung, Markus and Hibon, Pascale and Hung, Li-Wei and Ingraham, Patrick and Kalas, Paul and Konopacky, Quinn and Larkin, James E. and Maire, Jérôme and Marchis, Franck and Marley, Mark S. and Marois, Christian and Metchev, Stanimir and Millar-Blanchaer, Maxwell A. and Morzinski, Katie M. and Nielsen, Eric L. and Norton, Andrew and Oppenheimer, Rebecca and Palmer, David and Patience, Jennifer and Perrin, Marshall and Poyneer, Lisa and Rajan, Abhijith and Rameau, Julien and Rantakyrö, Fredrik T. and Sadakuni, Naru and Saddlemyer, Leslie and Savransky, Dmitry and Schneider, Adam C. and Serio, Andrew and Sivaramakrishnan, Anand and Song, Inseok and Soummer, Remi and Thomas, Sandrine and Wallace, J. Kent and Wang, Jason J. and Ward-Duong, Kimberly and Wiktorowicz, Sloane and Wolff, Schuyler (2017) '1–2.4 μm near-IR spectrum of the giant planet β Pictoris b obtained with the Gemini Planet Imager.', Astronomical journal., 153 (4). p. 182.

Abstract

Using the Gemini Planet Imager located at Gemini South, we measured the near-infrared (1.0–2.4 μm) spectrum of the planetary companion to the nearby, young star β 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 ${{ \mathcal M }}_{\mathrm{Jup}}$, an effective temperature of 1724 ± 15 K, a radius of 1.46 ± 0.01 ${{ \mathcal R }}_{\mathrm{Jup}}$, and a surface gravity of $\mathrm{log}g=4.18\pm 0.01$ [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 $\mathrm{log}g=3.5$–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 β 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.

Item Type:Article
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Status:Peer-reviewed
Publisher Web site:https://doi.org/10.3847/1538-3881/aa63e9
Publisher statement:© 2017. The American Astronomical Society. All rights reserved.
Date accepted:27 February 2017
Date deposited:11 July 2017
Date of first online publication:28 March 2017
Date first made open access:11 July 2017

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