deletions | additions       diff --git a/sectionMethdology_To.tex b/sectionMethdology_To.tex  index bebaca5..19eacfc 100644  --- a/sectionMethdology_To.tex  +++ b/sectionMethdology_To.tex 
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\item{Projected aspect ratio $\ge 50:1$}  \end{enumerate}  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: we will use the 8 \micron $\mu\textrm{m}$  imaging data from the GLIMPSE survey to create our own extinction maps, comparing these results with ones obtained from the lower 36\arcsec 36$''$c  resolution dust measurements  found in the Herschel column-density maps. 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, and 10}. 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.