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S.I. Young, R. Wilhelm (Texas Tech)
The blue horizontal branch stars have been valuable tracer probes of the halo field of our Galaxy. Despite widespread use, there exists only a few horizontal branch stars for which high resolution abundance analysis has been published. Increasing this number of stars can greatly help to identify abundance anomalies in the population, and add to the desperate need for abundance standards at fainter magnitudes.
We present results of a chemical abundance analysis for eight blue horizontal branch stars from the Beers, Preston, and Shectman HK objective-prism survey. The stars range in brightness from 11.9 < V < 12.7 and were observed at a resolution of R = 18,000. We have made use of the 2MASS JHK photometry to better constrain the temperatures of the program stars and the balmer line widths of the program stars taken at lower resolution (R=2000) in order to determine surface gravity. The analysis was done using Kurucz model atmospheres and the spectral synthesis routine, SPECTRUM, by Richard Gray. The abundance results for FeI, FeII, Ca, Ba, and Mg will be presented along with a comparison of abundance results for six standard HB stars. We will also look at possible abundance anomalies by comparing the determined [alpha/Fe] ratios.
The author(s) of this abstract have provided an email address for comments about the abstract: scott.i.young@ttu.edu
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Bulletin of the American Astronomical Society, 35#5
© 2003. The American Astronomical Soceity.