deletions | additions       diff --git a/spinning followup.tex b/spinning followup.tex  index e8adacb..eb92eb7 100644  --- a/spinning followup.tex  +++ b/spinning followup.tex 
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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. In this work we perform the expensive analysis task  of full parameter estimation that accounts for non-zero compact object spin. Whereas \citet{Singer_2014} used the (non-spinning) TaylorF2 waveform model, we make use of the SpinTaylorT4 waveform model \citep{Buonanno_2003,Buonanno_2009}, parameterized by the fifteen parameters that uniquely define a circularized compact binary inspiral. This analysis is perform on the 250 simulated sources from 2015 that \textsc{LALInference} was run on in \citet{Singer_2014}.  The simulated population of BNS systems contains slowly spinning NSs, with masses between $1.2~\mathrm{M}_\odot$ and $1.6~\mathrm{M}_\odot$ and spin magnitudes $\chi < 0.05$. This choice was motivated by the characteristics of NSs found thus far in BNS systems. 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 neutron-star equation of state (EOS) could theoretically have spins as high as $\chi \lesssim 0.7$ \citep{Lo_2011} without breaking up. For these reasons, the prior assumptions used for Bayesian inference of source parameters are more broad than the spin range of the simulated source population. 
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