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With the launch of JWST and other scheduled missions aimed at probing thedistant Universe, we are entering a new promising era for high-$z$ astronomy.One of our main goals is the detection of the first population of stars(Population III or Pop III stars), and models suggest that Pop III starformation is allowed well into the Epoch of Reionization (EoR), rendering thisan attainable achievement. In this paper, we focus on our chance of detectingmassive Pop IIIs at the moment of their death as Pair-Instability Supernovae(PISNe). We estimate the probability of discovering PISNe during the EoR ingalaxies with different stellar masses ($7.5 \leq\mathrm{Log}(M_\star/\mathrm{M_\odot}) \leq 10.5$) from six dustyGadgetsimulations of $50h^{-1}$ cMpc per side. We further assess the expected numberof PISNe in surveys with JWST/NIRCam and Roman/WFI. On average, less than onePISN is expected in all examined JWST fields at $z \simeq 8$ with $\Delta z =1$, and O(1) PISN may be found in a $\sim 1$ deg$^2$ Roman field in thebest-case scenario, although different assumptions on the Pop III IMF and/orPop III star-formation efficiency can decrease this number substantially.Including the contribution from unresolved low-mass halos holds the potentialfor increased discoveries. JWST/NIRCam and Roman/WFI allow the detection ofmassive-progenitor ($\sim 250 ~ \mathrm{M_\odot}$) PISNe throughout all theoptimal F200W-F356W, F277W-F444W, and F158-F213 colors. PISNe are alsopredominantly located at the outskirts of their hosting haloes, facilitatingthe disentangling of underlying stellar emission thanks to thespatial-resolution capabilities of the instruments.

The first fireworks: A roadmap to Population III stars during the Epoch of Reionization through Pair Instability Supernovae