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

  • Authors: Abhijith Rajan, Julien Rameau, Robert J. De Rosa, Mark S. Marley, James R. Graham, Bruce Macintosh, Christian Marois, Caroline Morley, Jennifer Patience, Laurent Pueyo, Didier Saumon, Kimberly Ward-Duong, S. Mark Ammons, Pauline Arriaga, Vanessa P. Bailey, Travis Barman, Joanna Bulger, Adam S. Burrows, Jeffrey Chilcote, Tara Cotten, Ian Czekala, Rene Doyon, Gaspard Duchêne, Thomas M. Esposito, Michael P. Fitzgerald, Katherine B. Follette, Jonathan J. Fortney, Stephen J. Goodsell, Alexandra Z. Greenbaum, Pascale Hibon, Li-Wei Hung, Patrick Ingraham, Mara Johnson-Groh, Paul Kalas, Quinn Konopacky, David Lafrenière, James E. Larkin, Jérôme Maire, Franck Marchis, Stanimir Metchev, Maxwell A. Millar-Blanchaer, Katie M. Morzinski, Eric L. Nielsen, Rebecca Oppenheimer, David Palmer, Rahul I. Patel, Marshall Perrin, Lisa Poyneer, Fredrik T. Rantakyrö, Jean-Baptiste Ruffio, Dmitry Savransky, Adam C. Schneider, Anand Sivaramakrishnan, Inseok Song, Rémi Soummer, Sandrine Thomas, Gautam Vasisht, J. Kent Wallace, Jason J. Wang, Sloane Wiktorowicz, and Schuyler Wolff

2017 The Astronomical Journal 154 10.

  • Provider: AAS Journals

Caption: Figure 7.

Comparison of the spectra, using the restricted fit, of the best-fitting T4.5 to T7.5 field brown dwarfs to 51 Eri b. The spectra shown in this figure are a subset of the data plotted in Figure 6. The brown dwarf spectral fits plotted here use the restricted chi-squared equations presented in Equation (2). The T4.5 and T5.0 spectra are from Looper et al. (2007), the T5.5 is from Burgasser et al. (2008), the T6.0 is from Burgasser et al. (2004), the T6.5 and T7.5 are from Burgasser et al. (2006), and the T7.0 is from Dupuy & Liu (2012).

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