Description
We present the quantitative methods used for selecting candidate metal-poor stars in the Hamburg/ESO objective-prism survey (HES). The selection is based on the strength of the CaII K line, B-V colors (both measured directly from the digital HES spectra), as well as J-K colors from the 2 Micron All Sky Survey. The KP index for CaII K can be measured from the HES spectra with an accuracy of 1.0{AA}, and a calibration of the HES B-V colors, using CCD photometry, yields a 1-sigma uncertainty of 0.07mag for stars in the color range 0.3<B-V<1.4.
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