We have developed a new procedure to search for carbon-enhanced metal-poor ( CEMP ) stars from the Hamburg/ESO ( HES ) prism-survey plates .
This method employs an extended line index for the CH G-band , which we demonstrate to have superior behavior when compared to the narrower G-band index formerly employed to estimate G-band strengths for these spectra .
Although CEMP stars have been found previously among candidate metal-poor stars selected from the HES , the selection on metallicity undersamples the population of intermediate-metallicity CEMP stars ( - 2.5 \leq [ Fe/H ] \leq - 1.0 ) ; such stars are of importance for constraining the onset of the s-process in metal-deficient asymptotic giant-branch stars ( thought to be associated with the origin of carbon for roughly 80 % of CEMP stars ) .
The new candidates also include substantial numbers of warmer carbon-enhanced stars , which were missed in previous HES searches for carbon stars due to selection criteria that emphasized stars with cooler temperatures .

A first subsample , biased towards brighter stars ( B < 15.5 ) , has been extracted from the scanned HES plates .
After visual inspection ( to eliminate spectra compromised by plate defects , overlapping spectra , etc. , and to carry out rough spectral classifications ) , a list of 669 previously unidentified candidate CEMP stars was compiled .
Follow-up spectroscopy for a pilot sample of 132 candidates was obtained with the Goodman spectrograph on the SOAR 4.1m telescope .
Our results show that most of the observed stars lie in the targeted metallicity range , and possess prominent carbon absorption features at 4300 Å .
The success rate for the identification of new CEMP stars is 43 \% ( 13 out of 30 ) for [ Fe/H ] < - 2.0 .
For stars with [ Fe/H ] < - 2.5 , the ratio increases to 80 \% ( 4 out of 5 objects ) , including one star with [ Fe/H ] < - 3.0 .