Mid-UV Determination of Ages and Metallicites of Elliptical Galaxies

Details Mid-UV Determination of Ages and Metallicites of Elliptical Galaxies Mid-UV Determination of Ages and Metallicites of Elliptical Galaxies

Dec 1997

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997aas...191.4902l&link_type=abstract

American Astronomical Society, 191st AAS Meeting, #49.02; Bulletin of the American Astronomical Society, Vol. 29, p.1291

Astronomy and Astrophysics

Astronomy

Scientific paper

Using simple population synthesis models, we have examined the mid-UV features of 11 nearby ellipticals and spiral bulges. The mid-UV (1800-3200 Angstroms ) for evolved stellar populations is dominated by light from the turn-off of the main sequence, unlike the optical region of the spectrum which is governed by the effective temperature of the red giant branch. By looking in the mid-UV and at the main sequence stars, we may break ``age-metallicity degeneracy'' (Worthey 1994) that plaques optical spectral synthesis models of evolved populations. In order to examine the spectral properties of only the main sequence stars, we have excluded P-AGB and EHB stars from our models' isochrones and have attempted to subtract out the hot component from the galaxies' spectra due to these far-UV emitting stars. Specifically, we measure the strength of the blend of FeI, SiI and SiIII at 2538 Angstroms (Bl2538) and introduce a new tool for examining the mid-UV continua, the slope of the continuum between 2600 and 3100 Angstroms (S2850). We find that populations older that 3 Gyr separate according to metallicity in the S2850 v. Bl2538 plane. Although globular cluster spectra agree with our single metallicity, single age populations, the spectral features of NGC 1399 require a multi-metallicity model including a small ( <= 10 % by mass) but mid-UV bright sub-component of low metallicity (Z <= 0.001) main sequence stars.

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