Optical Photometry of the New L Dwarf Spectral Sequence

Details Optical Photometry of the New L Dwarf Spectral Sequence Optical Photometry of the New L Dwarf Spectral Sequence

Feb 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999noao.prop..137g&link_type=abstract

NOAO Proposal ID #1999A-0137

Physics

Scientific paper

I propose to obtain VR photometry of the new spectral class cooler than M stars, the ``L dwarfs.'' These recently discovered field brown dwarf candidates are thought to have 1500 ≲ T_eff ≲ 2200 K. Models predict dust grain formation in these cool atmospheres, a conclusion supported by the observed depletion of Ti and V, but cannot predict the details of the grain size distribution. Optical photometry can constrain these models, since sub-micron grains will primarily affect the flux distribution at optical wavelengths. Observations of the methane brown dwarf Gl 229B and the L dwarf GD 165B suggest that the two objects have much different grain size distributions. The extremely red (V-K> 10) colors of these objects require the large aperture of WIYN.

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