deletions | additions       diff --git a/sectionMethdology_To.tex b/sectionMethdology_To.tex  index 5a15363..709c811 100644  --- a/sectionMethdology_To.tex  +++ b/sectionMethdology_To.tex 
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The name and coordinates for these ten filaments, along with their average LSR velocities, the number of bone criteria they satisfy, and a "quality rating" 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 $2 \times 10^{22}$ cm$^{-2}$, consistent with the minimum IRDC peak column density to be included in the \citet{Peretto_2009} catalog of 11,303 IRDCs. We calculate distances assuming all of our bone candidates (see Figure \ref{fig:skeleton}) are associated with the \citet{Dame_2011} Scutum-Centaurus arm. Two candidates, BC\_21.25-0.15 and BC\_11.13-0.12 show potential association with the Norma-4kpc arm; to confirm their distances, we use the the catalog from \citet{Ellsworth_Bowers_2013}, which provides distances to 1710 molecular clouds from the BGPS survey, derived using a Bayesian distance probability density function. The \citet{Ellsworth_Bowers_2013} derived distance to BC\_11.13-0.12 agrees with our \citet{Dame_2011} distance within estimated errors, while BC\_21.25-0.15 falls slightly outside the acceptable error range (see figure \ref{fig:mass_of_bones}).  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 even though it has  a velocity structure tangential $p-v$ orientation perpendicular  to predicted fits of the Scutum-Centaurus arm. arm (see Figure \ref{fig:skeleton}).  As spurs and interarm inter-arm  structures are likely to lie close to the physical Galactic midplane, mid-plane,  but with velocity gradients angled with respect to predicted arm fits, we also include this filament in attempt do {\it not} require that a bone be parallel  to classify all bones potentially aligned with Galactic structure---be it spiral arms, arm $p-v$ traces, so as not to exclude potential  spurs, feathers, or interarm regions. other inter-arm features.  Of the four remaining filaments that do not meet all six criteria---BC\_24.96-0.17, BC\_21.25-0.15, BC\_11.13-0.12, and BC\_357.62-0.33---all of them fail criterion 6 (aspect ratio $\ge 50:1$). As our criterion 6 does not allow for projection effects in imposing an aspect ratio limit, we emphasize that those filaments lying more tangential to our line-of-sight will appear foreshortened, and could very well meet the 50:1 minimum limit if projection effects were removed. We plan to examine the the aspect ratios (minus projection effects) of all our candidates in a follow-up study. Two of these filaments BC\_24.96-0.17 and BC\_357.62-0.33 show particular promise, both lying within 2-3 pc of the physical Galactic midplane (see appendix), though BC\_24.96-0.17 does lie at the upper limit of criterion 4, and its \citet{Ellsworth_Bowers_2013} derived distance places it 1 kpc closer than the distance derived from the \citet{Dame_2011} Scutum-Centaurus fit. The third filament, BC\_11.13-0.12 ("the snake"), has already been well-studied from a star formation perspective, hosting over a dozen protostellar cores likely to produce regions of high-mass star formation \citep{Wang_2014,Henning_2010}. From a Galactic bone perspective, the snake strongly satisfies all criteria except number 6---it lies within 15 pc of the physical galactic midplane and 5 km/s from the \citet{Dame_2011} Scutum-Centaurus global-log fit to CO, tracing a prominent peak of the Scutum-Centaurus arm in \textit{p-v} space (see appendix section BC\_11.13-0.12). The fourth filament, BC\_21.25-0.15 is arguably the weakest of all ten candidates: there is a slight break in the extinction feature near a longitude of $21.25^\circ$, and its placement in \textit{p-v} space suggests it is possibly an interarm filament (see appendix).