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Star formation is thought to be driven by two groups of mechanisms;spontaneous collapse and triggered collapse. Triggered star formationmechanisms further diverge into cloud-cloud collision (CCC), "collect andcollapse" (C\&C) and shock induced collapse of pre-existing, gravitationallystable cores, or 'radiation driven implosion' (RDI). To evaluate thecontributions of these mechanisms and establish whether these processes canoccur together within the same star forming region we performed mappingobservations of radio frequency ammonia, and water maser emission lines in theS235 massive star forming region. Via spectral analyses of main, hyperfine andmulti-transitional ammonia lines we explored the distribution of temperatureand column density in the dense gas in the S235 and S235AB star forming region.The most remarkable result of the mapping observations is the discovery of highdensity gas in inter-core bridges which physically link dense molecular coresthat house young proto-stellar clusters. The presence of dense gas implies thepotential for future star formation within the system of cores and gas bridges.Cluster formation implies collapse and the continuous physical links, also seenin re-imaged archival CS and $^{13}$CO maps, suggests a common origin to themolecular cores housing these clusters, i.e the structure condensed from asingle, larger parent cloud, brought about by the influence of a localexpanding H${\rm II}$ region. An ammonia absorption feature co-locating withthe center of the extended H${\rm II}$ region may be attributed to an older gascomponent left over from the period prior to formation of the H${\rm II}$region. Our observations also detail known and new sites of water maseremission, highlighting regions of active ongoing star formation.

NH$_3$ Observations of the S235 Star Forming Region: Dense Gas in Inter-core Bridges