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Ilya Mandel edited subsection_Luminosity_distance_label_sec__.tex
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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 \citep{Cutler_1994,Aasi_2013}, and the inclination can be better constrained for precessing 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
from 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
approximately scales with the distance, hence we divide the credible interval by the true (injected) distance
$D_\star$ $D_\star$; this gives an approximate analogue of twice the fractional uncertainty \citep{Berry_2014}. The cumulative distribution of the scaled credible intervals
are is plotted in figure \ref{fig:distance}. There is negligible difference between the spinning and non-spinning analyses as expected.