deletions | additions       diff --git a/sectionMethdology_To.tex b/sectionMethdology_To.tex  index d60f06c..4c8ddb4 100644  --- a/sectionMethdology_To.tex  +++ b/sectionMethdology_To.tex 
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By overlaying the HOPS, MALT90, BGPS, and GRS determined velocities on a \textit{p-v} diagram of CO emission, we establish whether these filaments are associated with an existing spiral arm trace. For this study, we use the whole-galaxy \citet{Dame_2001} CO survey to locate each of the arms in \textit{p-p-v} space and determine whether these filaments are consistent with global-log fits to CO and HI for various spiral arms. Of the approximately fifteen candidates identified visually, ten of these candidates are within 10 km/s of the Scutum-Centaurus and Norma-Cygnus arms. We plot these ten candidates in \textit{p-p-v} space 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}. We also include Scutum-Centaurus and Norma fits from Reid and Dame 2015 (in prep), derived from trigonometric parallax measurements of high-mass star forming regions taken as part of the BeSSeL survey \citep{Reid_2014}. Reid and Dame (2015), in prep, produce fits with ($l,b,v$) loci that closely follow GMCs that trace the arms, producing a rough log-spiral approximation determined by trigonometric parallax rather than an assumed galactic rotation curve.   \subsection{Establishing ``Bone" Criteria}  After narrowing down our list to ten filaments with kinematic structure consistent with existing spiral arm models, we develop a set ofquantitative  criteria for objects to be called "bones:" \begin{enumerate}  \item{Visually continuous mid-infrared extinction feature}