  We perform stellar evolution simulation of first stars and calculate stellar
yields from the first supernovae. The initial masses are taken from 12 to 140
Msun to cover the whole range of core-collapse supernova progenitors, and
stellar rotation is included, which results in efficient internal mixing. A
weak explosion is assumed in supernova yield calculations, thus only outer
distributed matter, which is not affected by the explosive nucleosynthesis, is
ejected in the models. We show that the initial mass and the rotation affect
the explosion yield. All the weak explosion models have abundances of [C/O]
larger than unity. Stellar yields from massive progenitors of > 40-60 Msun show
enhancement of Mg and Si. Rotating models yield abundant Na and Al. And Ca is
synthesized in non-rotating heavy massive models of > 80 Msun. We fit the
stellar yields to the three most iron-deficient stars, and constrain the
initial parameters of the mother progenitor stars. The abundance pattern in
SMSS 0313-6708 is well explained by 50-80 Msun non-rotating models, rotating
30-40 Msun models well fit the abundance of HE 0107-5240, and both non-rotating
and rotating 15-40 Msun models explain HE 1327-2326. The presented analysis
will be applicable to other carbon-enhanced hyper metal poor stars observed in
the future. The abundance analyses will give valuable information about the
characteristics about the first stars.
