All Tables

Table 1: Stellar parameters and chemical composition of HE 0107-5240 (Christlieb et al. 2004), and two theoretical models as explained in Sects. 2 (M 1) and 3 (M 2). The column "M 1 (initial)'' denotes the composition of the polluting SN ejecta; the interior of model M 1 has Z=0 throughout.
Table 2: Observational data for our selection of extremely metal-poor halo stars; HE 0107-5240 is repeated for completeness.
Table 3: Pop. II.5 models using the $M = 35~M_\odot$ SN yields of Chieffi & Limongi (2002). The mass cut has been found by inter- or extrapolating between SN models with different ${M_{\rm SN}({\rm Ni})}/{M_\odot }$ to obtain the correct ${\rm [C/Fe]}$ . ${M({\rm prim})}/{M({\rm SN})}$ is the mixing proportion between primordial and SN matter, needed to reach (approximately) the observed ${\rm [Fe/H]}$ -value. The various parameters of the models start at Col. 5 (age). Evolutionary models that could represent the objects are marked by the following labels: E-RGB: on RGB, but before bump; B-RGB: at bump; AB-RGB: after bump; L-RGB: close to tip; E-AGB: on early AGB, after 2nd dredge-up; L-AGB: immediately before thermal pulses commence; TP-AGB: thermal pulse phase on AGB. The last two lines refer to models for CS 22943-037, for which we have used alternative SN-yields from a $15~M_\odot$ model by Umeda & Nomoto 2002 (see text).