期刊
ASTRONOMICAL JOURNAL
卷 154, 期 1, 页码 -出版社
IOP Publishing Ltd
DOI: 10.3847/1538-3881/aa74e2
关键词
brown dwarfs; planetary systems; protoplanetary disks; stars: formation; stars: low-mass; stars: luminosity function, mass function; stars: pre-main sequence
资金
- National Science Foundation (NSF) [AST-1208239, AST-1313029]
- Space Telescope Science Institute [GO-11695]
- NASA NExSS program
- NASA [NAS 5-26555]
- NASA
- NSF
- Pennsylvania State University
- Eberly College of Science
- Pennsylvania Space Grant Consortium
- National Optical Astronomy Observatory (NOAO) [2015A-0175]
- U.S. Department of Energy
- U.S. National Science Foundation
- Ministry of Science and Education of Spain
- Science and Technology Facilities Council of the United Kingdom
- Higher Education Funding Council for England
- National Center for Supercomputing Applications at the University of Illinois at Urbana-Champaign
- Kavli Institute of Cosmological Physics at the University of Chicago
- Center for Cosmology and Astro-Particle Physics at the Ohio State University
- Mitchell Institute for Fundamental Physics and Astronomy at Texas AM University
- Financiadora de Estudos e Projetos
- Fundacao Carlos Chagas Filho de Amparo a Pesquisa do Estado do Rio de Janeiro
- Conselho Nacional de Desenvolvimento Cientifico e Tecnologico
- Ministerio da Ciencia, Tecnologia e Inovacao
- Deutsche Forschungsgemeinschaft
- Collaborating Institutions in the Dark Energy Survey
- [GS-2015A-Q-64]
We have performed a search for planetary-mass brown dwarfs in the Chamaeleon. I star-forming region using proper motions and photometry measured from optical and infrared images from the Spitzer Space Telescope, the Hubble Space Telescope, and ground-based facilities. Through near-IR spectroscopy at Gemini Observatory, we have confirmed six of the candidates as new late-type members of Chamaeleon I (>= M8). One of these objects, Cha J11110675-7636030, has the faintest extinction-corrected M-K among known members, which corresponds to a mass of 3-6 M-Jup according to evolutionary models. That object and two other new members have redder mid-IR colors than young photospheres at. <= M9.5, which may indicate the presence of disks. However, since those objects may be later than M9.5 and the mid-IR colors of young photospheres are ill-defined at those types, we cannot determine conclusively whether color excesses from disks are present. If Cha J11110675-7636030 does have a disk, it would be a contender for the least-massive known brown dwarf with a disk. Since the new brown dwarfs that we have found extend below our completeness limit of 6-10. M-Jup, deeper observations are needed to measure the minimum mass of the initial mass function in Chamaeleon. I.
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