Spectroscopy of L- and M- Dwarfs

Details Spectroscopy of L- and M- Dwarfs Spectroscopy of L- and M- Dwarfs

Dec 1998

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998aas...193.9805l&link_type=abstract

American Astronomical Society, 193rd AAS Meeting, #98.05; Bulletin of the American Astronomical Society, Vol. 30, p.1394

Astronomy and Astrophysics

Astronomy

Scientific paper

We have obtained infrared (1-2.5 microns) spectroscopy for 54 halo and disk stars around the stellar/substellar boundary. These data are combined with optical data where available and compared to synthetic spectra generated by the latest model atmospheres of Allard & Hauschildt. We find good agreement between observation and theory except for known problems in the V and H passbands probably due to incomplete molecular data for TiO, metal hydrides and H_2O. The metal-poor M subdwarfs are well matched by the models as oxide opacity sources are less important in this case. A version of the NextGen-Dusty models which includes homogeneous formation and extinction by dust grains produces a much improved match to the coolest objects in the sample, compared to the grainless models. Photospheric parameters - metallicity, effective temperature, radius - are determined for the sample. We present relationships between bolometric correction and color, and effective temperature and color, as a function of metallicity, and compare the radii and effective temperatures to recent structural models of low mass stars and brown dwarfs.

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