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UCHII regions are an important phase in the formation and early evolution ofmassive stars and a key component of the interstellar medium. The mainobjectives of this work are to study the young stellar objects (YSOs)associated with the G45.07+0.13 (G45.07) and G45.12+0.13 (G45.12) UCHIIregions, as well as the interstellar medium in which they are embedded. Wedetermined the distribution of the hydrogen column density (N(H2)) and dusttemperature (Td) in the molecular cloud using Herschel images. We used infraredphotometric data to identify and classify the YSOs. We also constructed acolour-magnitude diagram and K luminosity functions (KLFs) to compare theparameters of YSOs with the results of the radiative transfer models. We foundthat N(H2) varies from about 3.0 to 5.5x10^(23)cm^(-2) within the G45.07 andG45.12 regions, respectively. The maximum Td value is 35K in G45.12 and 42K inG45.07. Td reaches about 18-20K at distances of 2.6 and 3.7pc fromIRAS19110+1045 (G45.07) and IRAS19111+1048 (G45.12), respectively. The gas-dustmass value included in G45.12 is 3.4x10^5Msun and 1.7x10^5Msun in G45.07. TheUCHII regions are connected through a cold (Td=19K) bridge. The densitydistribution of 518 YSOs exhibits dense clusters around both IRAS sources. Theparameters of YSOs in the IRAS clusters (124 objects) and 394 non-clusterobjects surrounding them show some differences. About 75% of the YSOs belongingto the IRAS clusters have an evolutionary age greater than 10^6 years. Theirslope alpha of the KLF agrees well with a Salpeter-type Initial Mass Function(IMF) (gamma=1.35) for a high mass range (O-F stars, beta=2) at 1Myr. Thenon-cluster objects are uniformly distributed in the molecular cloud, 80% ofwhich are located to the right of the 0.1Myr isochrone. Based on the small agespread of the stellar objects, we suggest that the clusters originate from asingle triggering shock.

Infrared study of the star-forming region associated with the UC HII regions G45.07+0.13 and G45.12+0.13