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\section{Spinning Analysis}  \label{sec:spin}  \citet{Singer_2014} details the detection, low-latency localization, and medium-latency (i.e. non-spinning) follow-up of the simulated signals in 2015. Missing from the study is the complete characterization of sources, accounting for the spins of the NSs and their degeneracies with other parameters. In this work, we simulate this final step in the detection and characterization of BNS signals using the ``SpinTaylorT4'' fifteen-dimensional model for the GWs emitted by generically spinning, cicularized compact binary mergers \citep{Buonanno_2003,Buonanno_2009}.e  The simulated population of BNS systems contains very slowly spinning neutron stars, with spin magnitudes $\chi < 0.05$. This choice was motivated by the charactistics of neutron stars found in BNS systems to date. However, neutron stars \emph{outside} of BNS systems have been observed with spins as high as $\chi = 0.4$ \citep{Hessels_2006,Brown_2012}, and depending on the NS equation of state (EOS) could have spins as high as $\chi \lesssim 0.7$ \citep{Lo_2011} without breaking up. Thus, resticting priors to the narrow spin range used for the simulated population, could result in significant biases in parameter estimates if neutron stars with higher spins exist.