  We investigate the effect of the population III (Pop III) stars supernova
explosion~(SN) on the high redshifts reionization history with Planck latest
data. It is predicted that massive popIII stars~($130M_\odot\leq M\leq
270M_\odot$) explode energetically at the end of their stellar life as
pair-instability supernovae (PISNe). In the explosion, supernova remnants grow
as hot ionized bubbles and enhance the ionization fraction in the early stage
of the reionization history. This enhancement affects the optical depth of
cosmic microwave background~(CMB) and generates the additional anisotropy of
the CMB polarization on large scales. Therefore, analyzing the Planck
polarization data allows us to examine the Pop III star SNe and the abundance
of their progenitors, massive Pop III stars. In order to model the SN
contribution to reionization, we introduce a new parameter $\zeta$, which
relates to the abundance of the SNe to the collapse fraction of the Universe.
Using the Markov Chain Monte-Carlo method with the Planck latest polarization
data, we obtain the constraint "on our model parameter, $\zeta$." Our
constraint tells us that observed CMB polarization is consistent with the
abundance of PISNe predicted from the star formation rate and initial mass
function of Pop III stars in recent cosmological simulations. We also suggest
that combining further observations on the late reionization history such as
high redshift QSO observations can provide tighter constraints and important
information on the nature of Pop III stars.
