Figure 3 from DYNAMICAL MASS MEASUREMENT OF THE YOUNG SPECTROSCOPIC BINARY V343 NORMAE AaAb RESOLVED WITH THE GEMINI PLANET IMAGER

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DYNAMICAL MASS MEASUREMENT OF THE YOUNG SPECTROSCOPIC BINARY V343 NORMAE AaAb RESOLVED WITH THE GEMINI PLANET IMAGER

Authors: Eric L. Nielsen, Robert J. De Rosa, Jason Wang, Julien Rameau, Inseok Song, James R. Graham, Bruce Macintosh, Mark Ammons, Vanessa P. Bailey, Travis S. Barman, Joanna Bulger, Jeffrey K. Chilcote, Tara Cotten, Rene Doyon, Gaspard Duchêne, Michael P. Fitzgerald, Katherine B. Follette, Alexandra Z. Greenbaum, Pascale Hibon, Li-Wei Hung, Patrick Ingraham, Paul Kalas, Quinn M. Konopacky, James E. Larkin, Jérôme Maire, Franck Marchis, Mark S. Marley, Christian Marois, Stanimir Metchev, Maxwell A. Millar-Blanchaer, Rebecca Oppenheimer, David W. Palmer, Jenny Patience, Marshall D. Perrin, Lisa A. Poyneer, Laurent Pueyo, Abhijith Rajan, Fredrik T. Rantakyrö, Dmitry Savransky, Adam C. Schneider, Anand Sivaramakrishnan, Remi Soummer, Sandrine Thomas, J. Kent Wallace, Kimberly Ward-Duong, Sloane J. Wiktorowicz, and Schuyler G. Wolff

2016 The Astronomical Journal 152 175.

Provider: AAS Journals

Caption: Figure 3.

The best-fitting orbit (black) and 100 randomly selected orbits (blue) from the posterior distribution. The visual orbit is shown on the left, with solid lines connecting each data point to the location on the best-fitting orbit corresponding to the observing epoch. On the right are separation, position angle, and RV against time, with observed–calculated (O–C) residuals given below each plot, with respect to the best-fitting orbit. The combination of astrometry and RVs together provide a well-constrained orbit.

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