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We investigate the effect of the population III (Pop III) stars supernovaexplosion~(SN) on the high redshifts reionization history using the latestPlanck data. It is predicted that massive Pop~III stars~($130M_\odot\leq M\leq270M_\odot$) explode energetically at the end of their stellar life aspair-instability supernovae (PISNe). In the explosion, supernova remnants growas hot ionized bubbles and enhance the ionization fraction in the early stageof the reionization history. This enhancement affects the optical depth of thecosmic microwave background~(CMB) and generates the additional anisotropy ofthe CMB polarization on large scales. Therefore, analyzing the Planckpolarization data allows us to examine the Pop III star SNe and the abundanceof their progenitors, massive Pop III stars. In order to model the SNcontribution to reionization, we introduce a new parameter $\zeta$, whichrelates to the abundance of the SNe to the collapse fraction of the Universe.Using the Markov chain Monte Carlo method with the latest Planck polarizationdata, we obtain the constraint on our model parameter, $\zeta$. Our constrainttells us that observed CMB polarization is consistent with the abundance ofPISNe predicted from the star formation rate and initial mass function of PopIII stars in recent cosmological simulations. We also suggest that combiningfurther observations on the late reionization history such as high redshiftquasi-stellar object~(QSO) observations can provide tighter constraints andimportant information on the nature of Pop III stars.

Population III star explosions and Planck 2018 data