OGLE-2013-BLG-0911Lb: A Secondary on the Brown-Dwarf Planet Boundary around an M-dwarf
Abstract
We present the analysis of the binary-lens microlensing event OGLE-2013-BLG-0911. The best-fit solutions indicate the binary mass ratio of q~0.03 which differs from that reported in Shvartzvald+2016. The event suffers from the well-known close/wide degeneracy, resulting in two groups of solutions for the projected separation normalized by the Einstein radius of s~0.15 or s~7. The finite source and the parallax observations allow us to measure the lens physical parameters. The lens system is an M-dwarf orbited by a massive Jupiter companion at very close (M_{host}=0.30^{+0.08}_{-0.06} M_{Sun}, M_{comp}=10.1^{+2.9}_{-2.2} M_{Jup}, a_{exp}=0.40^{+0.05}_{-0.04} au) or wide (M_{host}=0.28^{+0.10}_{-0.08} M_{Sun}, M_{comp}=9.9^{+3.8}_{-3.5}M_{Jup}, a_{exp}=18.0^{+3.2}_{-3.2} au) separation. Although the mass ratio is slightly above the planet-brown dwarf (BD) mass-ratio boundary of q=0.03 which is generally used, the median physical mass of the companion is slightly below the planet-BD mass boundary of 13M_{Jup}. It is likely that the formation mechanisms for BDs and planets are different and the objects near the boundaries could have been formed by either mechanism. It is important to probe the distribution of such companions with masses of ~13M_{Jup} in order to statistically constrain the formation theories for both BDs and massive planets. In particular, the microlensing method is able to probe the distribution around low-mass M-dwarfs and even BDs which is challenging for other exoplanet detection methods.
Cite
@article{arxiv.1912.09613,
title = {OGLE-2013-BLG-0911Lb: A Secondary on the Brown-Dwarf Planet Boundary around an M-dwarf},
author = {Shota Miyazaki and Takahiro Sumi and David P. Bennett and Andrzej Udalski and Yossi Shvartzvald and Rachel Street and Valerio Bozza and Jennifer C. Yee and Ian A. Bond and Nicholas Rattenbury and Naoki Koshimoto and Daisuke Suzuki and Akihiko Fukui and F. Abe and A. Bhattacharya and R. Barry and M. Donachie and H. Fujii and Y. Hirao and Y. Itow and Y. Kamei and I. Kondo and M. C. A. Li and C. H. Ling and Y. Matsubara and T. Matsuo and Y. Muraki and M. Nagakane and K. Ohnishi and C. Ranc and T. Saito and A. Sharan and H. Shibai and H. Suematsu and D. J. Sullivan and P. J. Tristram and T. Yamakawa and A. Yonehara and J. Skowron and R. Poleski and P. Mr'oz and M. K. Szyma'nski and I. Soszy'nski and P. Pietrukowicz and S. KozLowski and K. Ulaczyk and L. Wyrzykowski and Matan Friedmann and Shai Kaspi and Dan Maoz and M. Albrow and G. Christie and D. L. DePoy and A. Gal-Yam and A. Gould and C. -U. Lee and I. Manulis and J. McCormick and T. Natusch and H. Ngan and R. W. Pogge and I. Porritt and Y. Tsapras and E. Bachelet and M. P. G. Hundertmark and M. Dominik and D. M. Bramich and A. Cassan and R. Figuera Jaimes and K. Horne and R. Schmidt and C. Snodgrass and J. Wambsganss and I. A. Steele and J. Menzies and S. Mao and U. G. Jorgensen and M. J. Burgdorf and S. Ciceri and S. Calchi Novati and G. D'Ago and D. F. Evans and T. C. Hinse and N. Kains and E. Kerins and H. Korhonen and L. Mancini and A. Popovas and M. Rabus and S. Rahvar and G. Scarpetta and J. Skottfelt and J. Southworth and G. D'Ago and N. Peixinho and P. Verma},
journal= {arXiv preprint arXiv:1912.09613},
year = {2020}
}
Comments
22 pages, 10 figures, Accepted for publication in The Astronomical Journal