deletions | additions       diff --git a/sectionMethdology_To.tex b/sectionMethdology_To.tex  index e2b5a53..5f53534 100644  --- a/sectionMethdology_To.tex  +++ b/sectionMethdology_To.tex 
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The name and coordinates for these ten filaments, along with their "nicknames", average LSR velocities, the bone criteria they satisfy, and their key defining features, are listed in figure \ref{fig:candidates}. In figure \ref{fig:mass_of_bones}, we summarize physical parameters for all ten bone candidates, including estimates of distance, volume, mass, and aspect ratio. We calculate mass by \textit{estimating} an average H$_2$ column density of $2\rm{E}22 \rm{cm}^{-2}$), consistent with the minimum IRDC peak column density to be included in the \citet{Peretto_2009} catalog of 11,303 IRDCs. We plan to directly measure this quantity in follow-up studies, using the 8 $\mu\textrm{m}$ imaging data from the GLIMPSE survey to create column density and temperature maps for our candidates.   Of the ten filaments with velocities consistent with galactic rotation, \textbf{six} of these meet all six bone criteria: \textbf{BC\_26.94-0.30, BC\_25.24-0.45,BC\_18.88-0.09, BC\_4.14-0.02, BC\_335.31-0.29, and BC\_332.21-0.04}, to varying degrees of excellence. We note that BC\_332.21-0.04 has likely been disrupted by stellar feedback, making its aspect ratio and velocity structure more difficult to define. Since we predict that all galactic bones will likely be destroyed by stellar feedback and/or galactic shear, we include it here as part of a larger attempt to build a catalog of bones at all stages of their evolution. We also include BC\_335.31-0.29, despite a velocity structure tangential to predicted fits of the Scutum-Centaurus arm. As spurs and interarm structures are likely to lie close to the physical Galactic midplane, but with velocity gradients angled with respect to predicted arm fits, we also include this filament in attempt to classify all bones potentially aligned wit with  Galactic structure. structure--be it spiral arms, spurs, feathers, or interarm regions.  Thus, it is important to note that some of the above criteria will likely be modified in the long run, as we learn more about the Skeleton of the Milky Way. Given our limited a priori knowledge of the Galaxy's structure, it is presently easier to find confirm  Bones that are spine-like, lying along arms with velocities predicted by extant modeling (criteria 1, 5), and harder to find spurs off those arms or inter-arm features, features (e.g. BC\_335.31-0.29),  the velocities of which are hard to predict well. Similarly, criterion 6 does not allow for projection effects in imposing an aspect ratio limit. As we learn more about spiral structure from simulations and modeling, these criteria will also be adjusted to allow for Bone-like features that represent spurs, inter-arm structures, and/or foreshortened structures lying close to our line of sight.