Removing a Major Uncertainty in Mass and Age Determinations of Young Stars

Details Removing a Major Uncertainty in Mass and Age Determinations of Young Stars Removing a Major Uncertainty in Mass and Age Determinations of Young Stars

Aug 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005noao.prop..416h&link_type=abstract

NOAO Proposal ID #2005B-0416

Physics

Scientific paper

Mass and age measurements of young stars rely on the stars' placement in an HR diagram relative to pre-main-sequence evolutionary tracks. Uncertainties in T_eff include a systematic error introduced by converting spectral types to T_eff according to a conversion scale derived from main-sequence stars. The advent of sophisticated synthetic spectra and modern molecular opacities offers us an opportunity to determine a new T_eff scale designed for young stars. We propose to measure T_eff for a large sample of non- accreting (weak-lined) T Tauri stars using low resolution red spectra on Goldcam. The resulting spectra will make it possible to estimate T_eff for any young star by simply finding the best spectral match with a star in our sample. This procedure will also work for accreting (classical) T Tauri stars, where weak-lined T Tauri stars are used as photospheric templates to distinguish stellar features from accretion signatures.

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