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We use NH3 inversion transitions to trace the dense gas in the NGC 1333region of the Perseus molecular cloud. NH3(1,1) and NH3(2,2) maps covering anarea of 102 square arcminutes at an angular resolution of ~3.7" are produced bycombining VLA interferometric observations with GBT single dish maps. Thecombined maps have a spectral resolution of 0.14 km/s and a sensitivity of 4mJy/beam. We produce integrated intensity maps, peak intensity maps anddispersion maps of NH3(1,1) and NH3(2,2) and a line-of-sight velocity map ofNH3(1,1). These are used to derive the optical depth for the NH3(1,1) maincomponent, the excitation temperature of NH3(1,1), and the rotationaltemperature, kinetic temperature and column density of NH3 over the mappedarea.  We compare these observations with the CARMA J=1-0 observations of N2H+ andH13CO+ and conclude that they all trace the same material in these dense starforming regions. From the NH3(1,1) velocity map, we find that a velocitygradient ridge extends in an arc across the entire southern part of NGC 1333.We propose that a large scale turbulent cell is colliding with the cloud, whichcould result in the formation of a layer of compressed gas. This region alongthe velocity gradient ridge is dotted with Class 0/I YSOs, that could haveformed from local overdensities in the compressed gas leading to gravitationalinstabilities. The NH3(1,1) velocity dispersion map also has relatively highvalues along this region, thereby substantiating the shock layer argument.

Connecting the Scales: Large Area High-resolution Ammonia Mapping of NGC 1333