Determining the Physical Properties of Very-Low-Mass Stars and Brown Dwarfs in the Near-Infrared

Details Determining the Physical Properties of Very-Low-Mass Stars and Brown Dwarfs in the Near-Infrared Determining the Physical Properties of Very-Low-Mass Stars and Brown Dwarfs in the Near-Infrared

Feb 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009aipc.1094..178r&link_type=abstract

COOL STARS, STELLAR SYSTEMS AND THE SUN: Proceedings of the 15th Cambridge Workshop on Cool Stars, Stellar Systems and the Sun.

Physics

Low Luminosity Stars, Subdwarfs, And Brown Dwarfs, Charge-Coupled Devices, Image Detectors, And Ir Detector Arrays, Star Formation

Scientific paper

Accurate measurements of the fundamental physical properties of very-low-mass stars and brown dwarfs are crucial for calibrating evolutionary models. Photometry and low-resolution spectroscopy effectively average over absorption features that sample different layers in complex cool atmospheres. By studying a large sample of objects bright enough for high-resolution spectroscopy, we can develop methods for determining physical properties as accurately and efficiently as possible. As part of the Brown Dwarf Spectroscopic Survey (BDSS [1, 2]), we are conducting a detailed comparison of observed and synthetic spectra for a sample of young M and L dwarfs and field M, L, and T dwarfs (~50 objects in total). High-resolution near-infrared spectra from NIRSPEC on Keck II provide an unequaled combination of resolving power and wavelength coverage. Synthetic spectra were created from PHOENIX atmosphere models calculated exclusively for this project with updated line lists and solar abundances. Combined with spectral types from photometric studies and low-resolution spectra and surface gravity estimates from age determination, the high-resolution spectra enable precise measurements of effective temperature and surface gravity, as well as accurate determination of radial velocity and projected rotational velocity. Our preliminary observation-model comparisons distinguish between wavelength regimes for which the models reproduce observed high-resolution spectra and regimes in which model data (line lists, oscillator strengths, etc.) are lacking.

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