Stromgren 4-color photometry of very metal-poor stars

Details Stromgren 4-color photometry of very metal-poor stars Stromgren 4-color photometry of very metal-poor stars

Nov 1998

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998larm.confe..99s&link_type=abstract

"IX Latin American Regional IAU Meeting, "Focal Points in Latin American Astronomy", held in Tonantzintla, Mexico, Nov 9-13, 199

Astronomy and Astrophysics

Astronomy

Scientific paper

Stromgren uvby photometry has been observed for an additional 140 very metal-poor stars from the survey of Beers et al. (1992). These Galactic stars of very-low metallicity provide crucial information for the investigation of the formation and evolution of the Galaxy, as well as on the nature of the early Universe. The Stromgren uvby$\beta$ system allows the measurement of stellar atmospheric parameters as a prelude to detailed abundance studies which will make use of high-resolution spectroscopy and the new generation of large telescopes. The photometric techniques developed by Schuster et al. (1996) are used not only to classify these very metal-poor stars but also to derive effective temperatures, surface gravities, and improve d estimates for their interstellar reddenings. In particular, photometric diagrams such as [$c1$], [$m1$] and $co$, $(b-y)o$ are used to classify these stars, especially those near the main-sequence turnoff, where contamination from slightly-evolved subgiants, lower surface-gravity horizontal-branch stars, and even a few supergiant or AGB candidates are found

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