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\section{Methodology}  To search for more bones, we visually inspected regions looked for them around  where arms they  are predicted expected  to lie in $l,b,v$ space, according to our current understanding of the Milky Way's structure. We began by calculating the expected ($l,b,v$) $l,b$  paths of Galactic arms using a log-spiral approximation as described in recent literature \cite{Dame_2011,Vallee_2008}, \cite{Dame_2011,Vallee_2008} and  assuming a 25 pc height above the plane for the Sun \citep[see][and references therein]{Goodman_2014}. The predicted positions of the Galactic arms (Scutum-Centaurus, Carina-Sagittarius, Norma-Cygnus, and Perseus) were then overlain on Spitzer GLIMPSE/MIPSGAL \citep{Benjamin_2003,Churchwell_2009} images in World Wide Telescope (WWT)---a tool that facilitates easy visualization of several layers of data at scales from the full sky down to the highest-resolution details. Panning along the full Spitzer/MIPSGAL Survey in WWT, we searched for largely continuous, filamentary, extinction features near and roughly parallel to the Galactic mid-plane, where all of the overlain arm traces lie. This visual inspection yielded about fifteen initial bone candidates. A video showing how this search worked in WWT is available \href{http://tinyurl.com/morenessies}{on YouTube}, and the original WWT Tour, of which the video shows a capture, is available at the \href{http://dx.doi.org/10.7910/DVN/29934}{Bones of the Milky Way Dataverse}. For features that appear associated with spiral arms on the 2-D plane of the sky, radial velocity data is needed to establish whether 3-D association with a spiral feature is likely. The filament Any good bone candidate  must have similar line-of-sight velocities along its length. Moreover, full length, and more importantly,  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 probe the velocity structure of these filaments, the initial bone candidates identified in WWT,  we employ employed  radial velocity data from five 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,Ellsworth_Bowers_2013}, GRS \citep{Jackson_2006} and ThrUMMS \cite{Barnes_2011}. 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 thesethermal emission  lines trace dense molecular gas ($\approx10^{4}\textrm{ cm}^{-3}$) cm}^{-3}$),  and are often found in dense, cool clouds with temperatures less than 100 K \citep{Purcell_2012,Shirley_2013}. As infrared dark clouds tend to harbor cool, high density clumps of gas which fuel the formation of massive stars, all three of these data sets contain spectra for hundreds of regions within the longitude range of the potential Galactic bones. To complement these high density gas tracers, we probe the puffier envelopes ($\approx10^{2}\textrm{ cm}^{-3}$) surrounding these bones using high resolution $^{13}\rm{CO}$ data from the GRS and ThrUMMS survey. We investigate the velocity structure of our filaments in two ways: first, whenever possible, we establish the velocity coherence of our candidates by performing a slice extraction along each filamentary extinction feature in \href{http://www.glueviz.org/en/stable/index.html}{Glue}, a visualization tool that facilitates the linking of data sets. We link spectral \textit{p-p-v} cubes from the GRS and ThrUMMS survey with GLIMPSE-Spitzer mid-infrared images and obtain velocity as a function of position along a path that traces the entire extinction feature. The results of the slice extraction along the path of one of our strongest bone candidates is shown in figure \ref{fig:filament5_slice}. We are able to establish velocity coherence for all candidates lying within the coverage range of the GRS survey ($ 18^\circ < l < 56^\circ$) and the ThrUMMS survey ($300^\circ < l < 358^\circ$). We also confirm that this GRS or ThrUMMS-determined velocity agrees with the velocity of dense gas tracers to within 5 km/s.