  We perform hydrodynamical and nucleosynthesis calculations of core-collapse
supernovae (SNe) and hypernovae (HNe) of Population (Pop) III stars. We provide
new yields for the main-sequence mass of $M_{\rm MS}=13-50$ $M_{\odot}$ and the
explosion energy of $E=1-40\times10^{51}$ ergs to apply for chemical evolution
studies. Our HN yields based on the mixing-fallback model of explosions
reproduce the observed abundance patterns of extremely metal-poor (EMP) stars
($-4< {\rm [Fe/H]}< -3$), while those of very metal-poor (VMP) stars ($-3<{\rm
[Fe/H]} < -2$) are reproduced by the normal SN yields integrated over the
Salpeter initial mass function. Moreover, the observed trends of abundance
ratios [X/Fe] against [Fe/H] with small dispersions for the EMP stars can be
reproduced as a sequence resulting from the various combination of $M_{\rm MS}$
and $E$. This is because we adopt the empirical relation that a larger amount
of Fe is ejected by more massive HNe. Our results imply that the observed
trends with small dispersions do not necessarily mean the rapid homogeneous
mixing in the early galactic halo at [Fe/H] $< -3$, but can be reproduced by
the ``inhomogeneous'' chemical evolution model. In addition, we examine how the
modifications of the distributions of the electron mole fraction $Y_{\rm e}$
and the density in the presupernova models improve the agreement with
observations. In this connection, we discuss possible contributions of
nucleosynthesis in the neutrino-driven wind and the accretion disk.
