on Keck I on 25 and 26 August 2001. A 0[${}^{\prime\prime}$]{}86 slit gave R$\sim$45,000. A blue setting which covered the wavelength 3190Å–4710Å was used for three observations of 1800s each. The second grating setting covered 3730Å–5275Å and was also used for three observations of 1800s. Exposures of a quartz lamp were used for flatfielding and of a ThAr lamp for wavelength calibration. The frame processing was done in IRAF[^2]. In addition to combining the three observations at each setting, we also combined all six observations together where they covered the same wavelengths. Our S/N ranged from $\sim$ 10 at 3200 Å to $\sim$80 at 4000Å to $\sim$ 100 at 5250Å. This star was also studied by A02, but at lower S/N and without the very blue wavelength coverage. They found that this star was extremely C- and N-rich, with \[C/Fe\]$=2.0$ and \[N/Fe\]$=1.2$ We were able to measure the abundances of several neutron-capture elements not included in the A02 study, and these provide interesting tests for theories of the origin of the heavy elements in the early Universe.

Abundance Analysis
==================

MOOG (Sneden 1973) was used for the abundance analysis. We used Kurucz[^3] (2003) model atmospheres. Our [T$_{\rm eff}$]{} comes from 