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\subsection{Spin Estimates}\label{sec:spin-magnitudes}  We now look at the constraints placed on the spin of the slowly spinning simulated BNS sources. Even though the simulations occupy avary  small fraction of the spin-magnitude  prior volume, most posterior distributions span the majority of the prior range for spin magnitudes. range.  For non-precessing systems with a relatively stationary systems, where the  orbital plane is stationary  with respect to the line-of-sight, varying the spin of the compact objects has a similar effect on the phase evolution of the GW as varying the mass ratio, resulting ratio. This results  in a strong degeneracy between the two parameters. Modulation of the GWs from precession of the orbital plane can break this degeneracy \citep{Vecchio_2004,Lang_2006,Vitale_2014,Chatziioannou_2014}, however \citep{Vecchio_2004,Lang_2006,Vitale_2014,Chatziioannou_2014}; however,  only systems with high large  spins that are misaligned with the orbital angular momentum significantly precess. Non-precessing systems, with either slow low  or aligned spins,only provide phase information and  suffer the most from this degeneracy. degeneracy as the only information regarding the mass and spin is encoded in the phase of the GW.  The simulated sources in this study fall in the latter category. category of low spins.  Figure (\ref{fig:spinPDF} \ref{fig:spinPDF}  or \ref{fig:spinPDFcred}) shows the distribution of PDFs for the spin of the most and least massive components, $\chi_1$ and $\chi_2$, respectively. The spin of the more massive component has a larger effect on the GW, and is therefore systematically better constrained, as seen in Fig. Figure  \ref{fig:spinPDF}. For both spins, however, the posterior shows slow spins to be only slightly more probable than high spins for most sources.