Simulations show that an IMF extending to at least 200 solar masses is required to match both the observed mass-metallicity-SFR relation and cosmic star formation history at z greater than or equal to 4, due to enhanced yields from pair-instability supernovae.
At each star for- mation timestep i, we first estimate the number of SN Ia pro- genitors expected to form as Ni Ia,P,est = NIaδM⋆ given the mass δMi ⋆ of stars formed in this step
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Impact of initial mass function on the chemical evolution of high-redshift galaxies
Simulations show that an IMF extending to at least 200 solar masses is required to match both the observed mass-metallicity-SFR relation and cosmic star formation history at z greater than or equal to 4, due to enhanced yields from pair-instability supernovae.