We have observed the massive star forming region , IRAS 18507 + 0121 , at millimeter wavelengths in 3 mm continuum emission and H ^ { 13 } CO ^ { + } ( J=1–0 ) and SiO ( v=0 , J=2–1 ) line emission , and at near-infrared wavelengths between 1.2 and 2.1 \mu m. Two compact molecular cores are detected : one north and one south separated by \sim 40 ^ { \prime \prime } .
The northern molecular core contains a newly discovered , deeply embedded , B2 protostar surrounded by several hundred solar masses of warm gas and dust , G34.4+0.23 MM .
Based on the presence of warm dust emission and the lack of detection at near-infrared wavelengths , we suggest that G34.4+0.23 MM may represent the relatively rare discovery of a massive protostar ( e.g .
analogous to a low-mass “ Class 0 ” protostar ) .
The southern molecular core is associated with a near-infrared cluster of young stars and an ultracompact ( UC ) HII region , G34.4 + 0.23 , with a central B0.5 star .
The fraction of near-infrared stars with excess infrared emission indicative of circumstellar material is greater than 50 % which suggests an upper limit on the age of the IRAS 18507 + 0121 star forming region of 3 Myrs .