deletions | additions       diff --git a/Filament selection and analysis.tex b/Filament selection and analysis.tex  index 1c50c94..27aeb7f 100644  --- a/Filament selection and analysis.tex  +++ b/Filament selection and analysis.tex 
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At 2.09 Myr we selected three filamentary features. Two are evolved versions of the features at 1.23 Myr (filaments C2 and D2), while filament E formed in the intervening time. At this point there are more sinks scattered through the box, including at least one in each of the filaments. The total sink mass is 92 M$_{\sun}$, i.e. an integrated star formation efficiency $\sim1.6\%$\footnote{We note in passing that this efficiency is a factor of 1.8 lower than the most equivalent simulation of \citet{2012ApJ...761..156F}, within the expected scatter resulting from different turbulent seeds, box sizes, and densities.}. We chose to analyse these early times, before the gas has begun converting to sinks in earnest, to approximate the evolutionary state of Hacar et al.'s observations.  UP TO HERE  \subsection{Line-of-sight velocity structure}  The rectangles surrounding the selected filaments define a coordinate system with axes aligned along the long axis or length $L$ of the filament, and the width $W$. The depth $D$ is the same axis that the surface density is projected along. We stepped along the $L$ and $W$ coordinates with a stepsize equal to the simulation's base resolution, and calculated at each point the density-weighted line-of-sight velocity integrated along the $D$ axis, using the same density range used to calculate the surface density. We binned these spectra into histograms with bin width 0.05 km s$^{-1}$.