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\subsection{Luminosity distance}\label{sec:distance}  The distance is more likely than the sky position to show the imprint of the spin. The distance is degenerate with the inclination, inclination \citep{Cutler_1994,Aasi_2013},  and the inclination can be better constrained for precessing systems. systems \citep{van_der_Sluys_2008,Vitale_2014}.  Since we are considering a population with low spins, precession is minimal, and there should be little effect including spin in the analysis. We quantify distance measurement accuracy using symmetric credible intervals: the distance credible interval $\mathrm{CI}_p^{D}$ in the range that contains the central $p$ of the integrated posterior, with $(1-p)/2$ falling both above and below the limits \citep{Aasi_2013}. The absolute size of the credible interval scales with the distance, hence we divide the credible interval by the true (injected) distance $D_\star$ this gives an approximate analogue of twice the fractional uncertainty \citep{Berry_2014}. The cumulative distribution of the scaled credible intervals are plotted in figure \ref{fig:dist}. \ref{fig:distance}.  There is negligible difference between the spinning and nonspinning analyses. analyses as expected.