Age and Abundance Discrimination in Old Stellar Populations Using Mid-Ultraviolet Colors

Details Age and Abundance Discrimination in Old Stellar Populations Using Mid-Ultraviolet Colors Age and Abundance Discrimination in Old Stellar Populations Using Mid-Ultraviolet Colors

2003-03-20

arxiv.org/abs/astro-ph/0303477v1

Astrophys.J. 591 (2003) 878-890

Astronomy and Astrophysics

Astrophysics

38 pages, 8 figures. Accepted by ApJ. Full resolution figures available at: http://www.astro.virginia.edu/~rwo/miduv-fullresfi

Scientific paper

10.1086/375413

The restframe mid-ultraviolet spectral region (2000-3200 A) is important in analyzing the stellar populations of the "red envelope" systems observed at high redshifts. Here, we explore the usefulness of the mid-UV for determining ages and abundances of old populations. A mid-UV to optical/IR wavelength baseline provides good separation of population components because the main sequence turnoff dominates the integrated light between 2500 and 4000 A. We find a six magnitude difference in the mid-UV continuum level over the metallicity range -1.5 < log Z/Z_o < +0.5 and a comparable difference (per unit log t) for ages in the range 4-16 Gyr. Logarithmic derivatives of mid-UV colors with respect to age or metal abundance are 3-10 times larger than for the UBV region. Most of the spectral information on old populations therefore resides below 4000 A. We investigate the capability of UBV and mid-UV broad-band colors to separately determine age and abundance, taking into account precision in the color measurements. We find that the mid-UV improves resolution in (log t,log Z) space by about a factor of 3 for a given observational precision. Contamination by hot horizontal branch phases can seriously affect mid-UV spectra, reaching over 80% in some cases. However, this is straightforward to remove as long as far-UV measurements are available. Finally, we show that a 4 Gyr, solar abundance model based on empirical spectra provides an excellent fit to the mid-UV spectrum of the E galaxy M32. This indicates that the poorer results obtained from theoretical spectra arise from limitations of the synthesis models for individual stars. [Condensed]

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