deletions | additions       diff --git a/sectionIntroduction_.tex b/sectionIntroduction_.tex  index 49caacf..9786770 100644  --- a/sectionIntroduction_.tex  +++ b/sectionIntroduction_.tex 
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Until very recently, no simulations had the spatial resolution to predict that super-dense filaments should trace the middle of spiral arms. In 2014, numerical simulations from \citet{Smith_2014}, using the AREPO moving mesh code, revealed dense filaments, with aspect ratios and column densities similar to Nessie, forming within and parallel to the mean plane of a simulated spiral galaxy. A detailed analysis of Nessie's properties, along with these new simulation results, suggests Nessie may be the first in a class of objects that could trace our Galaxy's densest spiral features \citep{Goodman_2014}. It is reassuring to recognize that Nessie should be the easiest object of its kind to find. Nessie is located in the closest major spiral arm to the the Sun, perpendicular to our line of sight, slightly offset from the Galactic center. This placement makes Nessie clearly visible against the bright background of the Galactic center, and more elongated than objects more distant or inclined to our line-of-sight.  In this paper, we use large-scale mid-infrared imaging of the Galactic plane to search for bone candidates near locations where currently-claimed spiral arms {\it should} lie on the sky (not exactly at b=0). $b=0$).  We investigate the best candidates' relationship to the Milky Way's spiral structure using molecular line data to establish likely distances. When used in conjunction with the kinematic, parallax, and extinction measurements outlined above, these new bones have the potential to pin down the Milky Way's galactic structure, improving the level of detail from tens of parsecs to around one parsec in regions near bones.