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\section{Introduction}   In recent years the focus of much star formation research has been on the relationship between the immediate star formation environment and the evolution of protostars. The data from the last generation of orbiting observatories has invigorated work toward understanding the formation of filamentary structures in molecular clouds, and the condensation of dense star forming cores form these filaments.  Recently \citet{http://www.aanda.org/articles/aa/abs/2013/06/aa20090-12/aa20090-12.html} presented observations of a prominent filamentary feature in Taurus, dominated by the L1495 cloud \citep{http://adsabs.harvard.edu/abs/1962ApJS....7....1L} \citep{1962ApJS....7....1L}  and the B213 dark patch \citep{http://adsabs.harvard.edu/abs/1927cdos.book.....B}. \citep{1927cdos.book.....B}.  Multiple velocity components along a single line of sight have also been observed in Serpens South \citep{http://adsabs.harvard.edu/abs/2013ApJ...778...34T}; \citep{2013ApJ...778...34T};  this feature may be common one in young star forming sites.