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Once star formation occurs, UV radiation in the Lyman–Werner
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star-forming regions. We reduce the effective star formation rate, but
the modelling does not depend on the environment. Further studies
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It is required that statistically reliable IMF information is examined
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Considering the effect of cosmic expansion for the IGM that the
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metals are expected to be observed as a localized absorber. In order
to estimate the accurate feasibility of detecting the metals taking
in such effects, further works of high spatial and time resolution
cosmological radiation hydrodynamic simulations are required.
We provide metal distribution originated in Pop III stars with
200 M or 30 M stars. This approach will be useful in expanding
our understanding of how the metals are distributed in the cosmic
volume. Although it has not been concluded that which mass
stars are typical or there exist several typical masses (e.g. Hirano
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of heavy elements than galactic metals in all our modellings. It
is essential whether we can distinguish the Pop III yield heavy
elements and galactic metals when we observe Pop III originated
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of SNe into account and confirm that the observed metals should
have a characteristic elemental abundance pattern, which is not
originated in galactic metals, even for partially contaminated cases.
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