deletions | additions       diff --git a/spinning followup.tex b/spinning followup.tex  index b6fc1a1..3aa1e73 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 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.\footnote{The fifteen parameters are two masses (either component masses or the chirp mass and mass ratio); six spin parameters describing the two spins (magnitudes and orientations); two coordinates for sky position; distance; an inclination angle; a polarization angle; a reference time, and the orbital phase at this time \citep[see][for more details]{Veitch_2015}. The masses and spins are intrinsic parameters which control the evolution of the binary, the others are extrinsic parameters which describe its orientation and position.} Furthermore, we We  assume the objects to be point masses with no tidal interactions. The estimation of tidal parameters using post-Newtonian approximations is rife with systematic uncertainties that are comparable in magnitude to statistical uncertainties \cite{Wade_2014}. Though marginalizing over uncertainties in tidal parameters can affect estimates of other parameters, the fact that tidal interactions only impact the evolution of the binary atvery  late times limits \citep[only having a masurable impact at frequencies above $\sim450~\mathrm{Hz}$;][]{Hinderer_2010}limits  both their measurability and the resulting biases in other parameter estimates caused by ignoring them \cite{Damour_2012}. 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 Galactic BNS systems expected to merge within a Hubble time through GW emission. 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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