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\citet{Watson2010} used 2MASS and GLIMPSE photometry and Spectral Energy Distribution (SED)-fitting to analyze the YSO population around 46 bubbles and found about a quarter showed an overabundance of YSOs near the boundary between the ionized interior and molecular exterior. These YSOs are candidates for being triggered by the expanding ionization and shock fronts created by the hot star. Star formation triggered by previous generations of stars is known to occur but the specific physical mechanism is still undetermined. The collect-and-collapse model \citep{Elmegreen1977} describes ambient material swept up by the shock fronts which eventually becomes gravitationally unstable, resulting in collapse. Other mechanisms, however, have been proposed. Radiatively-driven implosion \citep{1994A&A...289..559L}, for example, describes clumps already present in the ambient material whose contraction is aided by the external radiation of the hot star.  Bubbles with an overabundance of YSOs along the bubble-interstellar medium (ISM) boundary are a potentially excellent set of sources to study the mechanisms of triggered star-formation. The method of identifying YSOs through photometry, however, is limited. \citet{Robitaille_2006} showed that YSO age is degenerate with the observer's inclination angle. An early-stage YSO and a late-stage YSO seen edge on, so the accretion or debris disk is observed as thick and blocking the inner regions, can appear similar, even in the IR. Thus, we require other diagnostics of the YSOs along the bubble edge to determine the youngest, and most likely to have been triggered, YSOs. {\bf Additionally, a line-diagnostic allows us to rule out any line-of-sight coincidence associations.}  For the current project we selected a subset of the bubbles identified above to identify those YSOs associated with infall, outflows or hot cores by observing the CS (1-0) transition near 49 GHz with the Green Bank Telescope (GBT\footnote{The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc.}). CS is a probe of young star-formation. It has been detected in outflows from protostars, infall, disks and in hot cores \citep{1997A&A...317L..55D,1996A&AS..115...81B,Morata2012}. The chemistry is, naturally, complex, and it appears that CS can play several roles \citep{Beuther2002}, such as tracing outflows \citep{Wolf-Chase1998} or hot cores \citep{1997MNRAS.287..445C}. Our aim here is to use CS as a broad identifier of young star-formation and use any non-Gaussian line-shapes to infer molecular gas behavior.