Comparison of NH₃ and ¹²CO, ¹³CO, C¹⁸O Molecular Lines in the Aquila Rift Cloud Complex

The observations of the Aquila Rift cloud complex at 23.708 and 115.271 GHz made using the Nanshan 26 m radio telescope and the 13.7 m millimeter-wavelength telescope are presented. We find that the CO(1 − 0) gas distribution is similar to the NH 3 gas distribution in the Aquila Rift cloud complex. In some diffusion regions characterized by CO, we identified several dense clumps based on the distribution of detected ammonia molecular emission. Through the comparison of spectral line parameters for NH 3 , 13 CO, and C 18 O, our study reveals that the line center velocities of the NH 3 , 13 CO, and C 18 O lines are comparable and positively correlated, indicating that they originate from the same emission region. No significant correlation was identified for other parameters, including integrated intensity, line widths, main beam brightness temperature, as well as the column densities of NH 3 , 13 CO, and C 18 O. The absolute difference in line-center velocities between the 13 CO and NH 3 lines is less than both the average line width of NH 3 and that of 13 CO. This suggests that there are no significant movements of NH 3 clumps in relation to their envelopes. The velocity deviation is likely due to turbulent activity within the clumps.