Search and study of young infrared stellar clusters

The main aim of this paper is to study both the Interstellar Medium (ISM) and the young stellar population in the three star-forming regions, namely IRAS 05137+3919, 05168+3634, and 19110+1045. The study of the ISM includes determination of the hydrogen column density (N(H₂)) and dust temperature (T_d) in the regions using modified blackbody fitting. The main parameters of the identified and classified young stellar objects (YSOs) belonging to the regions were determined by comparing with the radiation-transfer models. We also constructed a color–magnitude diagram to compare the parameters of the YSOs with the results of the radiative-transfer models. The three stellar populations appear to have formed under different scenarios. In the cases of IRAS 05137+3919 and IRAS 05168+3634, the age spread is considerably wider, suggesting that the stellar population likely emerged from independent condensations. In contrast, the third region comprises a pair of ultracompact HII regions (UCHIIs), G45.12+0.13 and G45.07+0.13, with a notably smaller age spread. This hints at the possibility that these clusters originated from a single triggering event.