2017/12/02 by C. Dang-Duc, N. Phan-Bao, Dang-Duc, C. +1
Chemistry · Physics and Astronomy · #Astro and Planetary Science #Astronomy #Astrophysics #Astrophysics and Star Formation Studies #Astrophysics of Galaxies (astro-ph.GA) #Brown dwarf #FOS: Physical sciences #Galaxy #Low Mass #Mass distribution #Molecular Spectroscopy and Structure #Physics #Spectral energy distribution #Stars #Stellar classification #astro-ph.GA
paper · pdf · doi:10.48550/arxiv.1712.00597
Proceedings of the Star Formation in Different Environments, ICISE, Quy Nhon, Vietnam, 2016, (eds. D. Johnstone, T. Hoang, F. Nakamura, Q. Nguyen-Luong, and J. T. Tranh Van)
arxiv created 2017/12/02 · openalex publication_date 2017/12/02 · arxiv updated 2017/12/05 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/06
We report our study of two proto-brown dwarf candidates in Taurus, [GKH94]~41 and IRAS~04191+1523B. Based on continuum maps at 102~GHz (or 2.9~mm), spectral types and the spectral energy distribution of both targets, we confirmed the class I evolutionary stage of [GKH94]~41 and IRAS~04191+1523B, and estimated the upper limit to the final masses to be 49+56-27~M\rm J and 75+40-26~M\rm J for [GKH94]~41 and IRAS~04191+1523B, respectively. This indicates that they will likely end up as brown dwarfs or very low-mass stars. The existence of these class I very low-mass objects strongly supports the scenario that brown dwarfs and very low-mass stars have the same formation stages as low-mass stars.