deletions | additions       diff --git a/sectionMethdology_To.tex b/sectionMethdology_To.tex  index ba2c2a0..3fd9613 100644  --- a/sectionMethdology_To.tex  +++ b/sectionMethdology_To.tex 
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In figure \ref{fig:mass_of_bones}, we estimate physical parameters for our bones, including the aspect ratio, volume, $\rm{H}_2$ column density, and mass. We estimate an average density of $10^4 \rm{cm}^{-3}$, a more conservative estimate than the $10^5 \rm{cm}^{-3}$ estimate \citet{Goodman_2014} adopt for Nessie, chosen to produce a visual extinction of ∼ 100 magnitudes (consistent with the typical extinction on tenths of pc scales in an IRDC). We plan to directly measure these quantities in follow-up studies, using the 8 $\mu\textrm{m}$ imaging data from the GLIMPSE survey to create our 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{candidates 1, 3, 5, 7, 9, \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 10}. BC\_332.21-0.04}.  However, 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 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, 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.