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We surveyed the Aquila Rift complex including the Serpens South and W40region in the NH$_3$(1,1) and (2,2) transitions making use of the Nanshan 26-mtelescope. The kinetic temperatures of the dense gas in the Aquila Rift complexrange from 8.9 to 35.0K with an average of 15.3$\pm$6.1K. Low gas temperaturesassociate with Serpens South ranging from 8.9 to 16.8K with an average12.3$\pm$1.7K, while dense gas in the W40 region shows higher temperaturesranging from 17.7 to 35.0K with an average of 25.1$\pm$4.9 K. A comparison ofkinetic temperatures against HiGal dust temperatures indicates that the gas anddust temperatures are in agreement in the low mass star formation region ofSerpens South. In the high mass star formation region W40, the measured gaskinetic temperatures are higher than those of the dust. The turbulent componentof the velocity dispersion of NH$_3$(1,1) is found to be positively correlatedwith the gas kinetic temperature, which indicates that the dense gas may beheated by dissipation of turbulent energy. For the fractional total-NH3abundance obtained by a comparison with Herschel infrared continuum datarepresenting dust emission we find values from 0.1 to 21$\times 10^{-8}$ withan average of 6.9$(\pm 4.5)\times 10^{-8}$. Serpens South also shows afractional total-NH3 abundance ranging from 0.2 to 21$\times 10^{-8}$ with anaverage of 8.6($\pm 3.8)\times 10^{-8}$. In W40, values are lower, between 0.1and 4.3$\times 10^{-8}$ with an average of 1.6($\pm 1.4)\times 10^{-8}$. Weakvelocity gradients demonstrate that the rotational energy is a negligiblefraction of the gravitational energy. In W40, gas and dust temperatures are notstrongly dependent on the projected distance to the recently formed massivestars. Overall, the morphology of the mapped region is ring-like, with strongemission at lower and weak emission at higher Galactic longitudes.

Ammonia observations towards the Aquila Rift cloud complex