deletions | additions       diff --git a/Filament selection and analysis.tex b/Filament selection and analysis.tex  index d67c49a..b7775bb 100644  --- a/Filament selection and analysis.tex  +++ b/Filament selection and analysis.tex 
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\section{Filament selection and analysis}  After 1.25 Myr of self gravitating evolution, we selected by eye two filamentary features in one projection of the cloud's surface density, shown in figure \ref{finderimage}. In this image we plot the surface density calculated from contributions by gas in the range $10^3 < n/{\rm cm}^{-3} < 10^{4.5}$. This is roughly the density range traced by C$^{18}$O observations; we then convert the surface density to integrated line intensities. [SHOW EQUATION?] This approximate `observation' of our data yields an idea of what this simulation might look like in the motivating observations of \citet{2013A&A...554A..55H}. We chose one feature which, observationally speaking, would probably be deemed an obvious filament (the smaller feature to the lower right of figure \ref{finderimage}), and one that might be considered a ridge of star formation activity (the larger feature).  The boxes rectangular regions  surrounding the selected outline filaments define  a coordinate system oriented with axes aligned  along the long axis or length $L$ of the filament,the width $W$,  and the width $W$. The  depth $D$(which  is the same line of sight used in axis that  theprojected  surface density). density is projected along.  We stepped along the $L$ and $W$coordinates of the filaments  with step sizes corresponding a stepsize equal  to the simulations  base resolution of the simulation. At each location in the filament boxes we resolution, and  calculated at each point  the density-weighted line-of-sight velocity integrated  along the $D$ coordinate, again axis,  using the same density range used  to correspond to C$^{18}$O observations. This velocity spectrum was calculate the surface density. We  binned these spectra  into a histogram histograms  with bin width 0.05 km s$^{-1}$. s${-1}$.  In figure \ref{finderimage} we show thisvelocity  data on the  righthand side. We summed the histograms along the $W$ dimension, yielding the total velocity distribution along slices perpendicular to the filament's long axis.