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The formaldehyde $\rm H_2CO(1_{10} - 1_{11})$ absorption line andH$110\alpha$ radio recombination line (RRL) have been observed toward theAquila Molecular Cloud using the Nanshan 25 m telescope operated by theXinjiang Astronomical Observatory CAS. These first observations of the $\rmH_2CO$ $(1_{10} - 1_{11})$ absorption line determine the extent of themolecular regions that are affected by the ongoing star formation in the Aquilamolecular complex and show some of the dynamic properties. The distribution ofthe excitation temperature $T_{ex}$ for $\rm H_2CO$ identifies the two knownstar formation regions W40 and Serpens South as well as a smaller new regionSerpens 3. The intensity and velocity distributions of $\rm H_2CO$ and $\rm^{13}CO(1-0)$ do not agree well with each other, which confirms that the $\rmH_2CO$ absorption structure is mostly determined by the excitation of themolecules resulting from the star formation rather than by the availability ofmolecular material as represented by the distribution. Some velocity-coherentlinear $\rm ^{13}CO(1-0)$ structures have been identified in velocity channelmaps of $\rm H_2CO$ and it is found that the three star formation regions lieon the intersect points of filaments. The $\rm H110\alpha$ emission is foundonly at the location of the W40 H II region and spectral profile indicates aredshifted spherical outflow structure in the outskirts of the H II region.Sensitive mapping of $\rm H_2CO$ absorption of the Aquila Complex has correctlyidentified the locations of star-formation activity in complex molecular cloudsand the spectral profiles reveal the dominant velocity components and mayidentify the presence of outflows.

$\rm H_2CO$ and $\rm H110\alpha$ Observations toward the Aquila Molecular Cloud