期刊
ASTRONOMY & ASTROPHYSICS
卷 548, 期 -, 页码 -出版社
EDP SCIENCES S A
DOI: 10.1051/0004-6361/201220182
关键词
brown dwarfs; stars: low-mass; techniques: photometric; techniques: spectroscopic; infrared: stars; surveys
资金
- Ramon y Cajal fellowship [08-303-01-02]
- Spanish ministry of science and innovation [AYA2010-19136]
- FONDECYT [3100098, 3110004]
- Joint Committee ESO-Government of Chile
- CONICYT
- Center for Astrophysics FONDAP
- Proyecto Basal PB06 (CATA)
- Spanish Ministry of Economics and Competitiveness
- Fondo Europeo de Desarrollo Regional FEDER [AYA2010-21308-C03-02, AYA2010-21308-C03-03, AYA2010-20535]
- RoPACS
- National Aeronautics and Space Administration
- National Science Foundation
- Alfred P. Sloan Foundation
- US Department of Energy
- Japanese Monbukagakusho
- Max Planck Society
- Higher Education Funding Council for England
- Science and Technology Facilities Council [ST/H004157/1, PP/C002229/1, ST/H00243X/1, ST/J00541X/1, ST/H004165/1, ST/G002622/1, ST/J000647/1, ST/J001546/1, ST/K000217/1, ST/J001538/1] Funding Source: researchfish
- STFC [ST/F002831/1, ST/H004165/1, ST/G002622/1, ST/J00541X/1, ST/K000217/1, ST/J001538/1, ST/J001546/1, ST/H004157/1, PP/C002229/1, ST/J000647/1] Funding Source: UKRI
Aims. The aim of the project is to improve our current knowledge of the density of T dwarfs and the shape of the substellar initial mass function by identifying a magnitude-limited sample of T dwarfs in the full southern sky. Methods. We present the results of a photometric search aimed at discovering cool brown dwarfs in the southern sky imaged at infrared wavelengths by the Visible and Infrared Survey Telescope for Astronomy (VISTA) and the Wide Infrared Survey Explorer (WISE) satellite mission. We combined the first data release (DR1) of the VISTA Hemisphere Survey (VHS) and the WISE preliminary data release to extract candidates with red mid-infrared colours and near-to mid-infrared colours characteristics of cool brown dwarfs. Results. The VHS DR1 vs. WISE search returned tens of T dwarf candidates, 13 of which are presented here, including two previously published in the literature and five new ones confirmed spectroscopically with spectral types between T4.5 and T8. We estimate that the two T6 dwarfs lie within 16 pc and the T4.5 within 25 pc. The remaining three are 30-50 pc distant. The only T7 dwarf in our sample is the faintest of its spectral class with J = 19.28 mag. The other six T dwarf candidates remain without spectroscopic follow-up. We also improve our knowledge on the proper motion accuracy for three bright T dwarfs by combining multi-epoch data from public databases (DENIS, 2MASS, VHS, WISE, Spitzer).
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