Polarisation of very-low-mass stars and brown dwarfs
I. VLT/FORS1 optical observations of field ultra-cool dwarfsB. Goldman1, J. Pitann1, M. R. Zapatero Osorio2, C. A. L. Bailer-Jones1, V. J. S. Béjar2, J. A. Caballero3, and Th. Henning1
1 Max Planck Institute for Astronomy, Königstuhl 17, 69117 Heidelberg, Germany
2 Instituto de Astrofísica de Canarias, C/ Vía Lactéa S/N, 38205 La Laguna, Tenerife, Spain
3 Departamento de Astrofísica, Facultad de Ciencias Físicas, Universidad Complutense de Madrid, 28040 Madrid, Spain
Received 14 October 2008 / Accepted 5 April 2009
Context. Ultra-cool dwarfs of the L spectral type ( = 1400–2200 K) are known to have dusty atmospheres. Asymmetries of the dwarf surface may arise from rotationally-induced flattening and dust-cloud coverage, and may result in non-zero linear polarisation through dust scattering.
Aims. We aim to study the heterogeneity of ultra-cool dwarfs' atmospheres and the grain-size effects on the polarisation degree in a sample of nine late M, L and early T dwarfs.
Methods. We obtain linear polarimetric imaging measurements using FORS1 at the Very Large Telescope, in the Bessel I filter, and for a subset in the Bessel R and the Gunn z filters.
Results. We measure a polarisation degree of (0.310.06)% for LHS102BC. We fail to detect linear polarisation in the rest of our sample, with upper-limits on the polarisation degree of each object of 0.09% to 0.76% (95% of confidence level), depending on the targets and the bands. For those targets we do not find evidence of large-scale cloud horizontal structure in our data. Together with previous surveys, our results set the fraction of ultra-cool dwarfs with detected linear polarisation to % (1- errors). From the whole sample of well-measured objects with errors smaller than 0.1%, the fraction of ultra-cool dwarfs with polarisation degree larger than 0.3% is smaller than 16% (95% confidence level).
Conclusions. For three brown dwarfs, our observations indicate polarisation degrees different (at the 3- level) than previously reported, giving hints of possible variations. Our results fail to correlate with the current model predictions for ultra-cool dwarf polarisation for a flattening-induced polarisation, or with the variability studies for a polarisation induced by an heterogeneous cloud cover. This stresses the intricacy of each of those tasks, but may arise as well from complex and dynamic atmospheric processes.
Key words: stars: low-mass, brown dwarfs -- stars: atmospheres -- polarization -- stars: individual: LHS 102B
© ESO 2009