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We present a 1D LTE chemical abundance analysis of the very bright (V=9.1)Carbon-Enhanced Metal-Poor (CEMP) star BD +44 493, based on high-resolution,high signal-to-noise spectra obtained with Subaru/HDS. The star is shown to bea subgiant with an extremely low iron abundance ([Fe/H]=-3.7), while it is richin C ([C/Fe]=+1.3) and O ([O/Fe]=+1.6). Although astronomers have beensearching for extremely metal-poor stars for decades, this is the first starfound with [Fe/H]<-3.5 and an apparent magnitude V<12. Based on its lowabundances of neutron-capture elements (e.g., [Ba/Fe]=-0.59), BD +44 493 isclassified as a "CEMP-no" star. Its abundance pattern implies that afirst-generation faint supernova is the most likely origin of its carbonexcess, while scenarios related to mass loss from rapidly-rotating massivestars or mass transfer from an AGB companion star are not favored. From ahigh-quality spectrum in the near-UV region, we set an very low upper limit onthis star's beryllium abundance (A(Be)=log(Be/H)+12<-2.0), which indicates thatthe decreasing trend of Be abundances with lower [Fe/H] still holds at[Fe/H]<-3.5. This is the first attempt to measure a Be abundance for a CEMPstar, and demonstrates that high C and O abundances do not necessarily implyhigh Be abundances.

BD +44 493: A Ninth Magnitude Messenger from the Early Universe; Carbon Enhanced and Beryllium Poor