i et al. (2017), which is arrived from Madau &amp; Dickinson (2014) with the inclusion of the metallicity dependence of the star formation rate, which is bassically the effect related to pair-instability supernova (PSN) and pair-instability pulsation supernova (PPSN).</p></li>
</ul>
<p><span class="math">\begin{equation}
\mathcal{R}_m(z_s) = \frac{\mathcal{R}_O(b_4+1)e^{b_2 z_s}}{b_4+e^{b_3 z_s}} \text{Gpc}^{-3}\text{yr}^{-1} \tag{1}
\end{equation}</span> * <span class="math notranslate nohighlight">\(z_s\)