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We compare elemental abundance patterns of $\sim 200$ extremely metal-poor(EMP; [Fe/H]$<-3$) stars with supernova yields of metal-free stars in order toobtain insights into the characteristic masses of the first (Population III orPop III) stars in the Universe. Supernova yields are prepared withnucleosynthesis calculations of metal-free stars with various initial masses($M=$13, 15, 25, 40 and 100 $M_{\odot}$) and explosion energies($E_{51}=E/10^{51}$[erg]$=0.5-60$) to include low-energy, normal-energy, andhigh-energy explosions. We adopt the mixing-fallback model to take into accountpossible asymmetry in the supernova explosions and the yields that best-fit theobserved abundance patterns of the EMP stars are searched by varying the modelparameters. We find that the abundance patterns of the EMP stars arepredominantly best-fitted with the supernova yields with initial masses $M<40M_{\odot}$, and that more than than half of the stars are best fitted with the$M=25 M_\odot$ hypernova ($E_{51}=10$) models. The results also indicate thatthe majority of the primordial supernovae have ejected $10^{-2}-10^{-1}M_\odot$ of $^{56}$Ni leaving behind a compact remnant, either a neutron staror a black hole, with mass in a range of $\sim 1.5-5 M_{\odot}$. The resultssuggest that the masses of the first stars responsible for the firstmetal-enrichment are predominantly $< 40 M_{\odot}$. This implies that thehigher mass first stars were either less abundant or directly collapsing into ablackhole without ejecting heavy elements or that a supernova explosion of ahigher-mass first star inhibits the formation of the next generation oflow-mass stars at [Fe/H]$<-3$.

The Initial mass function of the first stars inferred from extremely metal-poor stars