Astrometric confirmation and preliminary orbital parameters of the young exoplanet 51 eridani b with the gemini planet imager

Robert J D De Rosa, Eric L. Nielsen, Sarah C. Blunt, James R. Graham, Quinn M. Konopacky, Christian Marois, Laurent Pueyo, Julien Rameau, Dominic M. Ryan, Jason J. Wang, Vanessa Bailey, Ashley Chontos, Daniel C. Fabrycky, Katherine B. Follette, Bruce MacIntosh, Franck Marchis, S. Mark Ammons, Pauline Arriaga, Jeffrey K. Chilcote, Tara H. CottenRené Doyon, Gaspard Duchene, Thomas M. Esposito, Michael P. Fitzgerald, Benjamin Gerard, Stephen J. Goodsell, Alexandra Z. Greenbaum, Pascale Hibon, Patrick Ingraham, Mara Johnson-Groh, Paul G. Kalas, David Lafreniere, Jerome Maire, Stanimir Metchev, Maxwell A. Millar-Blanchaer, Katie M. Morzinski, Rebecca Oppenheimer, Rahul I. Patel, Jennifer Patience, Marshall D. Perrin, Abhijith Rajan, Fredrik T. Rantakyrö, Jean Baptiste Ruffio, Adam C. Schneider, Anand Sivaramakrishnan, Inseok Song, Debby Tran, Gautam Vasisht, Kimberly Ward-Duong, Schuyler G. Wolff

Research output: Contribution to journalArticle

27 Scopus citations

Abstract

We present new Gemini Planet Imager observations of the young exoplanet 51 Eridani b that provide further evidence that the companion is physically associated with 51 Eridani. Combining this new astrometric measurement with those reported in the literature, we significantly reduce the posterior probability that 51 Eridani b is an unbound foreground or background T-dwarf in a chance alignment with 51 Eridani to 2 × 10-7, an order of magnitude lower than previously reported. If 51 Eridani b is indeed a bound object, then we have detected orbital motion of the planet between the discovery epoch and the latest epoch. By implementing a computationally efficient Monte Carlo technique, preliminary constraints are placed on the orbital parameters of the system. The current set of astrometric measurements suggest an orbital semimajor axis of AU, corresponding to a period of years (assuming a mass of 1.75 Mo for the central star), and an inclination of deg. The remaining orbital elements are only marginally constrained by the current measurements. These preliminary values suggest an orbit that does not share the same inclination as the orbit of the distant M-dwarf binary, GJ 3305, which is a wide physically bound companion to 51 Eridani.

Original languageEnglish (US)
Article numberL3
JournalAstrophysical Journal Letters
Volume814
Issue number1
DOIs
StatePublished - Nov 20 2015

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Keywords

  • planetary systems
  • planets and satellites: detection
  • stars: individual (51 Eri)

ASJC Scopus subject areas

  • Astronomy and Astrophysics
  • Space and Planetary Science

Cite this

De Rosa, R. J. D., Nielsen, E. L., Blunt, S. C., Graham, J. R., Konopacky, Q. M., Marois, C., Pueyo, L., Rameau, J., Ryan, D. M., Wang, J. J., Bailey, V., Chontos, A., Fabrycky, D. C., Follette, K. B., MacIntosh, B., Marchis, F., Ammons, S. M., Arriaga, P., Chilcote, J. K., ... Wolff, S. G. (2015). Astrometric confirmation and preliminary orbital parameters of the young exoplanet 51 eridani b with the gemini planet imager. Astrophysical Journal Letters, 814(1), [L3]. https://doi.org/10.1088/2041-8205/814/1/L3