  We present a chemical abundance analysis of the faint halo metal-poor
main-sequence star J0023+0307, with [Fe/H]<-6.3, based on a high-resolution
(R~35,000) Magellan/MIKE spectrum. The star was originally found to have
[Fe/H]< -6.6 based on a Ca II K measurement in an R~2,500 spectrum. No iron
lines could be detected in our MIKE spectrum. Spectral lines of Li, C, Na, Mg,
Al, Si, and Ca were detected. The Li abundance is close to the Spite Plateau,
A(Li) = 1.7, not unlike that of other metal-poor stars although in stark
contrast to the extremely low value found e.g., in HE~1327-2326 at a similar
[Fe/H] value. The carbon G-band is detected and indicates strong C-enhancement,
as is typical for stars with low Fe abundances. Elements from Na through Si
show a strong odd-even effect, and J0023+0307 displays the second-lowest known
[Ca/H] abundance. Overall, the abundance pattern of J0023+0307 suggests that it
is a second-generation star that formed from gas enriched by a massive
Population III first star exploding as a fall-back supernova The inferred
dilution mass of the ejecta is 10^(5+-0.5) Msun of hydrogen, strongly
suggesting J0023+0307 formed in a recollapsed minihalo. J0023+0307 is likely
very old because it has a very eccentric orbit with a pericenter in the
Galactic bulge.
