object ($\chi_1=0.998,\chi_2=0$). The choice $\chi_i=0.998$ corresponds to the [@Thorne:1974ve] bound. This value of the spin is outside the regime in which phenomenological models have been calibrated, and it has been chosen to provide rough upper limits on the rates.](fig-mma-paper-SNRVersusMass){width="\columnwidth"}

Figure \[fig:Ingredients:SNRVersusMass:CompareModels\] shows that these models all make similar predictions for the SNR of optimally oriented equal-mass binaries as a function of their total mass for a single aLIGO detector. Even small differences can be important: for any given binary, a $30\%$ difference in amplitude corresponds to a factor $(1.3)^3\simeq 2.2$ in rate calculations. In practice, however, all nonspinning IMR models agree in SNR to within tens of percent over the total binary mass range of interest (up to $127\msun$, see Section \[dcos\]). The effect of spin will be discussed in more detail in Section \[subsec:WF\] below.

![image](AdLIGOZDHP_20Hz_SNR100Mpc_ins.ps){width="1.0\columnwidth"} ![image](AdLIGOZDHP_20Hz_SNR100Mpc_IMR.ps){width="1.0\columnwidth"}

![image](AdLIGOZDHP_20Hz_DLhor_ins.ps){width="1.0\columnwidth"} ![image](AdLIGOZDHP_20Hz_DLhor_IMR.ps){width="1.0\columnwidth"}\

Figure \[fig:Ingredients:SNRContours\] shows contour plots of the SNR, $\rho$, in the $(M_z, q)$ plane, where $M_z \equiv M(1+z)$ is the redshifted total mass, $z$ is the redshift, and $q=m_2/m_1 \leq 1$ is the mass ratio of the components, for nonspinning binaries at luminosity distance $D_L=100$ Mpc. We discuss the justification for considering the SNR as a function of $M_z$ below, 