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\section{Introduction}  Massive stars strongly influence their surrounding environment. The two most important mechanisms before their post-main-sequence evolution are through bipolar outflows during formation and ionizing radiation during their main-sequence. This influence was observed in the form of bubble-shaped emission in the 8 $\mu$m band of the  Spitzer-GLIMPSE survey of the Galactic Plane (Benjamin et al. 200X). Churchwell et al. (2006, 2007) observed bubble-shaped 8 $\mu$m emission to be common throughout the Galactic plane. Watson et al. (2008, 2009) found 24 $\mu$m and 20 cm emission centered within the 8 $\mu$m emission and interpreted the objects as caused by hot stars ionizing their surroundings, creating 20 cm free-free emission, and at larger distances exciting PAHs, creating 8 $\mu$m emission. Anderson et al. (2011) also interpreted these as classical HII regions. Watson et al. (2010) used 2MASS and GLIMPSE photometery 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 interesting because they 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 (citation?) but the specific physical mechanism is still undetermined. The collect-and-collapse model (Elmegreen \& Lada, 1977) describes the ambient material swept up by the shock fronts as eventually becoming gravitationally unstable, resulting in collapse. Other mechanisms, however, have been proposed. Radiatively-driven implosion (Lefloch \& Lazareff, 1994), for example, described ambient material as an already existent clump, but whose contraction is aided by the external radiation of the hot star.  
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The current project aimed to identify the youngest YSOs by observing the CS (1-0) transition near 49 GHz with the Green Bank Telescope (GBT). CS is a probe of young star-formation. It has been detected in outflows from protostars, infall and in hot cores (citations?). The chemistry is, naturally, complex, and it appears that CS can play several roles. 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.   After describing the survey and mapping observations (sec 2) and numerical results (sec 3), we analyze the Herschel-HiGAL emission toward all our sources to determine, along with our CS detections, the CS abundances (sec 4.1). We also analyze three sources for evidence of rapid infall (sec 4.2) and the mapped regions. We end with a summary of the conclusions.