Disentangling Metallicity and Age for Turnoff Stars

Details Disentangling Metallicity and Age for Turnoff Stars Disentangling Metallicity and Age for Turnoff Stars

Jul 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999ap%26ss.265..427p&link_type=abstract

Astrophysics and Space Science, v. 265, Issue 1/4, p. 427-430 (1999).

Astronomy and Astrophysics

Astrophysics

Scientific paper

This is a progress report on calculations of near-ultraviolet spectrawith Ben Dorman at NASA/Goddard, for the ultimate purpose of extractingage and metallicity from extragalactic spectra. We are calculating fromfirst principles a grid of spectra covering 2200-3400 Å using theKurucz program SYNTHE, beginning with stars of metallicity less thanone-fifth solar ([Fe/H] < -0.7). For these stars, LTE calculationsusing known opacities and line lists including only transitions measuredin the laboratory, coupled with standard line-blanketed LTE models, providea satisfactory match to the spectra of turnoff stars of temperaturesT eff = 5750 K - 6250 K. For more metal-rich stars, two problemsarise: lines without a laboratory identification become increasinglyinfluential, and the cores of all strong lines become too strong. Theseproblems must be addressed to match near-UV spectra of turnoff stars ofsolar metallicity or higher.

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