We present results of an analysis of high-resolution spectra ( R \sim 50 000 ) , obtained with the Subaru Telescope High Dispersion Spectrograph , of two Carbon-Enhanced Metal-Poor ( CEMP ) stars selected from the Hamburg/ESO prism survey , HE 1305 + 0007 and HE 1152 - 0355 , and of the classical CH star HD 5223 .
All of these stars have relatively low effective temperatures ( 4000–4750 K ) and high carbon abundances , which results in the presence of very strong molecular carbon bands in their spectra .
The stellar atmospheric parameters for these stars indicate that they all have surface gravities consistent with a present location on the red-giant branch , and metallicities of { [ Fe / H ] } = -2.0 ( HE 1305 + 0007 , HD 5223 ) and { [ Fe / H ] } = -1.3 ( HE 1152 - 0355 ) .
In addition to their large enhancements of carbon ( { [ C / Fe ] } = +1.8 , +1.6 and +0.6 .
respectively ) , all three stars exhibit strong enhancements of the s-process elements relative to iron .

HE 1305 + 0007 exhibits a large enhancement of the 3rd-peak s-process element lead , with { [ Pb / Fe ] } = +2.37 , as well as a high abundance of the r-process element europium , { [ Eu / Fe ] } = +1.97 .
The 2nd-peak s-process elements Ba , La , Ce , Nd , and Sm are found to be more enhanced than the 1st-peak s-process elements Zr , Sr and Y .
Thus , HE 1305 + 0007 joins the growing class of the so-called “ Lead Stars ” , and also the class of objects that exhibit the presence of both r-process and s-process elements , the CEMP-r/s stars .
The large enhancement of n-capture elements exhibited by HE 1152 - 0355 and HD 5223 are more consistent with the abundance patterns generally noticed in CH stars , essentially arising from pure s-process nucleosynthesis .
The elemental abundance distributions observed in these stars are discussed in the light of existing theories of CH star formation , as well as the suggested formation scenarios of the CEMP-r/s group .