Adam J. Burgasser, Mike A. Lopez, Eric E. Mamajek, Jonathan Gagné, Jacqueline K. Faherty, Melisa Tallis, Caleb Choban, Tomoki Tamiya, Ivanna Escala, Christian Aganze
2016 Astrophysical Journal  
The 32 Orionis group is a co-moving group of roughly 20 young (24 Myr) M3-B5 stars 100 pc from the Sun. Here we report the discovery of its first substellar member, WISE J052857.69+090104.2. This source was previously reported to be an M giant star based on its unusual near-infrared spectrum and lack of measurable proper motion. We re-analyze previous data and new moderate-resolution spectroscopy from Magellan/FIRE to demonstrate that this source is a young near-infrared L1 brown dwarf with
more » ... low surface gravity features. Spectral model fits indicate T_eff = 1880^+150_-70 K and g = 3.8^+0.2_-0.2 (cgs), consistent with a 15-22 Myr object with a mass near the deuterium-burning limit. Its sky position, estimated distance, kinematics (both proper motion and radial velocity), and spectral characteristics are all consistent with membership in 32 Orionis, and its temperature and age imply a mass (M = 14^+4_-3 M_Jup) that straddles the brown dwarf/planetary-mass object boundary. The source has a somewhat red J-W2 color compared to other L1 dwarfs, but this is likely a low-gravity-related temperature offset; we find no evidence of significant excess reddening from a disk or cool companion in the 3-5 μm waveband.
doi:10.3847/0004-637x/820/1/32 fatcat:sexoyrwu4rewfjx3mqwn2ljere