  We present a detailed chemical abundance analysis of HE 1300+0157, a subgiant
with [Fe/H]=-3.9. From a high-resolution, high-S/N Subaru/HDS spectrum we find
the star to be enriched in C ([C/Fe]_1D ~ +1.4) and O ([O/Fe]_1D ~ +1.8). With
the exception of these species, HE 1300+0157 exhibits an elemental abundance
pattern similar to that found in many other very and extremely metal-poor
stars. The Li abundance is lower than the Spite-plateau value, in agreement
with expectation for its evolutionary status. Of particular interest, no
neutron-capture elements are detected in HE 1300+0157. This type of abundance
pattern has been found by recent studies in several other metal-poor giants. We
suggest that HE 1300+0157 is an unevolved example of this group of stars, which
exhibit high C abundances together with low (or absent) abundances of
neutron-capture elements. Several potential enrichment scenarios are presented.
The low neutron-capture elements, including Sr, Ba, and Pb, suggests that the
carbon excess observed in HE 1300+0157 is not due to mass transfer across a
binary system. Such a scenario is applied to carbon-rich objects with excesses
of s-process elements. The normal observed Li abundance supports this
interpretation. Most likely, the high levels of C and O were produced prior to
the birth of this star. It remains unclear whether a single hypernova is
responsible for its overall chemical pattern, or whether one requires a
superposition of yields from a massive Population III object and a normal Type
II SN. These scenarios provide important information on the C production in the
early Universe, and on the formation of C-rich stars in the early Galaxy.
