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We present combined interferometer and single dish telescope data of NH3(J,K) = (1,1) and (2,2) emission towards the clustered star forming OphiuchusB, C and F Cores at high spatial resolution (~1200 AU) using the AustraliaTelescope Compact Array, the Very Large Array, and the Green Bank Telescope.While the large scale features of the NH3 (1,1) integrated intensity appearsimilar to 850 micron continuum emission maps of the Cores, on 15" (1800 AU)scales we find significant discrepancies between the dense gas tracers in OphB, but good correspondence in Oph C and F. Using the Clumpfind structureidentifying algorithm, we identify 15 NH3 clumps in Oph B, and 3 each in Oph Cand F. Only five of the Oph B NH3 clumps are coincident within 30" (3600 AU) ofa submillimeter clump. We find v_LSR varies little across any of the Cores, andadditionally varies by only ~1.5 km/s between them. The observed NH3 linewidths within the Oph B and F Cores are generally large and often mildlysupersonic, while Oph C is characterized by narrow line widths which decreaseto nearly thermal values. We find several regions of localized narrow lineemission (\Delta v < 0.4 km/s), some of which are associated with NH3 clumps.We derive the kinetic temperatures of the gas, and find they are remarkablyconstant across Oph B and F, with a warmer mean value (T_K = 15 K) thantypically found in isolated regions and consistent with previous results inclustered regions. Oph C, however, has a mean T_K = 12 K, decreasing to aminimum T_K = 9.4 K towards the submillimeter continuum peak, similar toprevious studies of isolated starless cores. There is no significant differencein temperature towards protostars embedded in the Cores. [Abridged]

The Initial Conditions of Clustered Star Formation I: NH3 Observations of Dense Cores in Ophiuchus