deletions | additions       diff --git a/sectionMethdology_To.tex b/sectionMethdology_To.tex  index 6031c8f..a47dece 100644  --- a/sectionMethdology_To.tex  +++ b/sectionMethdology_To.tex 
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\section{Methodology}  To search for more bones, we visually inspect regions (|$l$|\textless 30$^{\circ}$, |$b$|\textless 1$^{\circ}$) where arms are predicted to lie according to our current understanding of the Milky Way's structure; the expected ({\it l,b,v}) ($l,b,v$)  paths of the Galactic arms are calculated using a log-spiral approximation as described in recent literature \cite{Dame_2011, Vallee_2008}. The predicted positions of the Galactic arms (Scutum-Centaurus, Carina-Sagittarius, Norma-Cygnus, and Perseus) are overlaid on three-color Spitzer GLIMPSE \citep{Benjamin_2003,Churchwell_2009} images in World Wide Telescope---a tool that facilitates easy visualization of several layers of data at scales from the full sky down to the highest-resolution details. As part of our initial criteria, we search for long, largely continuous, filamentary mid-infrared extinction features that are near and roughly parallel to the Galactic mid-plane. This initial inspection yielded about fifteen Bone candidates (a video showing how this search worked in WWT is available at tinyurl.com/morenessies). Regardless of this initial visual inspection, the true nature of these filaments, and their association with a spiral feature, can only be established by looking at radial velocity data. The filament must have similar line-of-sight velocities along its length to ensure its contiguity. Moreover, the measured radial velocities should be very close to those predicted by the Milky Way's rotation curve for arms at a known distance. To investigate the velocity structure of these fifteen filaments, we employ radial velocity data from four separate radio surveys: HOPS \citep{Purcell_2012,Walsh_2011}, MALT90 \citep{Foster_2011,Jackson_2013}, BGPS spectral line follow-up \cite{Schlingman_2011,Shirley_2013} and GRS \citep{Jackson_2006}. The HOPS, MALT90, and BGPS surveys are all geared towards probing dense regions hosting the early stages of high mass star formation. We utilize $\textrm{NH}_3$ emission from HOPS, $\mathrm{N_2H^{+}}$ from MALT90, and $\textrm{HCO}^{+}$ from BGPS. All three of these thermal emission lines trace dense molecular gas ($\approx10^{4}\textrm{ cm}^{-3}$) and are often found in dense, cool clouds with temperatures less than 100 K \citep{Purcell_2012, Shirley_2013}. As infrared dark clouds tend to harbor cool, high density clumps of gas which fuel the formation of massive stars, all three of these data sets contain spectra for hundreds of regions within the longitude range of the potential Galactic bones.