deletions | additions       diff --git a/sectionMethdology_To.tex b/sectionMethdology_To.tex  index 963480a..dd80491 100644  --- a/sectionMethdology_To.tex  +++ b/sectionMethdology_To.tex 
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In cases where HOPS, MALT90, and BGPS catalog data are not available along the extinction feature, we were also able to extract spectra from GRS (high resolution $^{13}$CO (1-0) data) and MALT90 p-p-v cubes using the spectrum extracter tool in Glue. A demonstration of the procedure used to extract velocities in Glue is shown in figure \ref{fig:glue}. As CO traces lower density gas (on average $10^2 \textrm{ cm}^{-3}$) and $\mathrm{N_2H+}$, HCO$^+$, and $\textrm{NH}_3$ trace high density gas ($>10^4 \textrm{ cm}^{-3}$), the dense gas sources provide much stronger evidence for the velocity of cold, dense, filamentary IRDCs. When dense gas sources were not available, the complete and unbiased high resolution GRS survey, although less desirable, allows us to roughly gauge the velocity along entire lengths of filaments. In filaments composed entirely of GRS spectra, we took HOPS spectra over the entire filament using Glue and confirmed that this HOPS-determined velocity agreed with GRS-determined average velocity to within 5 km/s. In the future, we hope to take higher resolution spectra of high density tracers to better pinpoint the velocity of these IRDCs.   By overlaying the HOPS, MALT90, BGPS, and GRS determined velocities on a p-v diagram of CO emission, we determine whether these filaments are physical spines or simply a chance projection of mid-infrared extinction features along our line-of-sight. For this study, we use the whole-galaxy \citet{Dame_2001} CO survey to locate each of the arms in p-p-v space. Of the approximately fifteen candidates identified visually, ten of these candidates are within 10 km/s of the Scutum-Centaurus and Norma-Cygnus arms. The central coordinates for these ten filaments, along with their average lengths, LSR velocities, and distances, are listed in table \ref{tab:candidates}. We plot these ten candidates in p-p-v space, as shown in figure \ref{fig:skeleton}. In addition to showing our Bone candidates, we show several different predictions of the positions of two spiral arms toward the inner Galaxy in longitude-velocity space, from \citet{Dame_2011}, \citet{Sanna_2014}, \citet{Shane_1972}, and \citet{Vallee_2008}. For reference, we note that the new BeSSeL (maser) results from \citet{Sato_2014} in the first quadrant favor the oldest, HI-based \citet{Shane_1972}, fits for the Scutum arm. After narrowing down our list to ten filaments with kinematic structure consistent with Galactic rotation, we develop a set of quantitative criteria for objects to be called "bones:"  \begin{enumerate}  \item{Largely continuous mid-infrared extinction feature}  \item{Roughly parallel to the Galactic plane}  \item{Within 20 pc of the physical Galactic mid-plane}  \item{Within 10 km/s of the global-log spiral fit to any Milky Way arm}  \item{No abrupt shifts in velocity (of more than ~3 km/s per 10 pc) within extinction feature}  \item{Projected aspect ratio $\ge 50:1$}  \end{enumerate}  We calculate the aspect ratios and masses per unit length for all ten filaments, along with other parameters, which are summarized in 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{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***INVALID BYTE SEQUENCE HERE***' 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.