OGLE-2016-BLG-1266: A Probable Brown Dwarf/Planet Binary at the Deuterium Fusion Limit

May 2018 • 2018ApJ...858..107A

Authors • Albrow, M. D. • Yee, J. C. • Udalski, A. • Calchi Novati, S. • Carey, S. • Henderson, C. B. • Beichman, C. • Bryden, G. • Gaudi, B. S. • Shvartzvald, Y. • Spitzer Team • Szymański, M. K. • Mróz, P. • Skowron, J. • Poleski, R. • Soszyński, I. • Kozłowski, S. • Pietrukowicz, P. • Ulaczyk, K. • Pawlak, M. • OGLE Collaboration • Chung, S. -J. • Gould, A. • Han, C. • Hwang, K. -H. • Jung, Y. K. • Ryu, Y. -H. • Shin, I. -G. • Zhu, W. • Cha, S. -M. • Kim, D. -J. • Kim, H. -W. • Kim, S. -L. • Lee, C. -U. • Lee, D. -J. • Lee, Y. • Park, B. -G. • Pogge, R. W. • KMTNet Collaboration

Abstract • We report the discovery, via the microlensing method, of a new very low mass binary system. By combining measurements from Earth and from the Spitzer telescope in Earth-trailing orbit, we are able to measure the microlensing parallax of the event, and we find that the lens likely consists of a (12.0 ± 0.6)M J + (15.7 ± 1.5)M J super-Jupiter/brown dwarf pair. The binary is located at a distance of 3.08 ± 0.18 kpc in the Galactic plane, and the components have a projected separation of 0.43 ± 0.03 au. Two alternative solutions with much lower likelihoods are also discussed, an 8M J and 6M J model and a 90M J and 70M J model. If all photometric measurements were independent and Gaussian distributed with known variances, these alternative solutions would be formally disfavored at the 3σ and 5σ levels. We show how the more massive of these models could be tested with future direct imaging.


IPAC Authors


Sebastiano Calchi Novati

Associate Scientist

Sean Carey

Senior Scientist