but since the chosen distance corresponds to a negligible redshift $z\simeq 0.023$ using the cosmological parameters $\Omega_M=0.3$, $\Omega_\Lambda=0.7$, $\Omega_{\rm k}=0$, and $h=0.7$ (chosen for consistency with [@dominik; @dominik2]), $M\simeq M_z$ at this distance. The left panel refers to a calculation using an inspiral-only waveform with Newtonian amplitude to compute the horizon distance. The right panel includes inspiral, merger, and ringdown, modelled using the PhC waveform. This plot shows two important features: (1) including the full IMR increases the maximum SNR at this luminosity distance by factors of a few with respect to an inspiral-only calculation, from $\approx 300$ to $\approx 10^3$; (2) high-mass binaries ($M_z \gtrsim
10^{2.5}M_\odot \approx 300 M_\odot$) involving BHs that would not be detectable using inspiral waveforms, become detectable using IMR waveforms. The latter point is not important for the field binaries considered in this paper, but it is crucial for intermediate-mass BH mergers [e.g., @walczak; @Fregeau:2006; @Amaro:2006imbh].

In an expanding Universe, GW emission is redshifted by the same factor of $(1+z)$ as electromagnetic radiation. In the units ($G=c=1$) adopted by relativists to describe gravitational waves, the only quantity with dimensions in the GW signal is the total mass $M$. Since the total mass sets the time 