the frequency domain is well approximated by the quadrupole formula, i.e., $\tilde h(f)\sim \mc^{5/6} f^{-7/6}/D$. Here $D$ is the luminosity distance to the source. The estimate of Eq. (\[eq:LocalUniverseMergerRateFormula\]) follows from this simple scaling together with the definition of the SNR, Eq. (\[SNR\]).

![\[fig:noise\] **Noise models**: we use an analytical approximation to the aLIGO zero-detuning high power (ZDHP) noise power spectral density given in Eq. (4.7) of [@ajithspin] (we verified that this approximation gives results in excellent agreement with the “official” tabulated aLIGO ZDHP noise PSD given in [@PSD:AL]. For AdV we use the fit in Eq. (3.4) of [@ajithbose] to [@AdvVirgo], and for KAGRA we use the PSD fit from the Appendix of [@pannarale] to [@KAGRA].](noise){width="1.0\columnwidth"}

Eq. (\[eq:LocalUniverseMergerRateFormula\]) involves only the *local* merger rate ${\cal R}(0)$ and $\langle \mc^{15/6}\rangle$ is averaged over detected binaries. Both quantities can easily be extracted from [StarTrack]{} simulations; they are listed in Table \[tab:simplerates\], along with the values of $R_D$ predicted by Eq. (\[eq:LocalUniverseMergerRateFormula\]). We expect this rough estimate to be accurate for NS-NS binaries, for which the overwhelming majority of the SNR is accumulated during the inspiral phase. More accurate calculations are required for DCOs comprised of BHs, because they are visible out 