Calibrating models of ultralow-mass stars

Details Calibrating models of ultralow-mass stars Calibrating models of ultralow-mass stars

2005-10-17

arxiv.org/abs/astro-ph/0510502v1

Astronomy and Astrophysics

Astrophysics

4 pages, accepted for AN, "Ultra low mass star formation and evolution"

Scientific paper

10.1002/asna.200510433

Evolutionary and atmospheric models have become available for young ultralow-mass objects. These models are being used to determine fundamental parameters from observational properties. TiO bands are used to determine effective temperatures in ultralow-mass objects, and together with Na- and K-lines to derive gravities at the substellar boundary. Unfortunately, model calibrations in (young) ultralow-mass objects are rare. As a first step towards a calibration of synthetic spectral features, I show molecular bands of TiO, which is a main opacity source in late M-dwarfs. The TiO $\epsilon$-band at 8450\AA is systematically too weak. This implies that temperatures determined from that band are underestimated, and I discuss implications for determining fundamental parameters from high resolution spectra.

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