Physical parameters of T dwarfs derived from high-resolution near-infrared spectra

Details Physical parameters of T dwarfs derived from high-resolution near-infrared spectra Physical parameters of T dwarfs derived from high-resolution near-infrared spectra

2009-03-25

arxiv.org/abs/0903.4461v1

Astronomy and Astrophysics

Astrophysics

Solar and Stellar Astrophysics

27 pages, 17 figures, A&A, in press

Scientific paper

We determine the effective temperature, surface gravity and projected rotational velocity of nine T dwarfs from the comparison of high-resolution near-infrared spectra and synthetic models, and estimate the mass and age of the objects from state-of-the-art models. We use the AMES-COND cloudless solar metallicity models provided by the PHOENIX code to match the spectra of the T dwarfs observed with the NIR high-resolution spectrograph NIRSPEC using ten echelle orders to cover part of the J band from 1.165 to 1.323 microns with R~20,000. The projected rotational velocity, Teff and logg of the objects are determined based on the minimum RMS of the differences between the modelled and observed relative fluxes. The modelled spectra reproduce quite well the observed features for most of the T dwarfs, with Teff in the range of 922-1009 K, and logg between 4.3 and 5 (cm s^-2). Our results support the assumption of a dust free atmosphere for T dwarfs later than T5, where dust grains form and then gravitationally sediment into the low atmosphere. The modelled spectra do not accurately mimic some individual very strong lines like the KI doublet at 1.2436 and 1.2525 microns. Our modelled spectra does not match well the observed spectra of the two T dwarfs with earlier spectral types, namely SDSSp J125453.90-012247.4 (T2) and 2MASS J05591914-1404488 (T4.5), which is likely due to the presence of condensate clouds that are not incorporated in the models used here. By comparing our results and their uncertainties to evolutionary models, we estimate masses in the interval ~5-75 MJ for T dwarfs later than T5, which are in good agreement with those found in the literature. We found apparent young ages that are typically between 0.1 and a few Gyr for the same T dwarfs, which is consistent with recent kinematical studies.

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