reveals the radio continuum counterparts of most of the optical features indicated in Fig. 2. In particular, the brightest  regions G353.2+0.9 and G353.1+0.6, which were studied by @felli90 at 5.0 GHz, are easily identified. On the contrary, G353.2+0.7 (centered at 172535.52, –3416546), which was also investigated by @felli90, can not be identified in the radio continuum image as a distinct physical structure. The western border of this feature, as delineated by @felli90, is part of G353.12+0.86, while the eastern section may be part of G353.24+0.64 or of the large shell, as pointed out by @felli90. The radio counterpart of the shell-like structure G353.12+0.86 is first identified. The radio emitting region at 1725, –341220, located slightly to the southeast of the  region G353.2+0.9, lacks an optical counterpart.

The upper panel of Fig. \[IR-1\] shows the distribution of the dust colour temperature T$_c$ (in contours and grayscale), while an overlay of the H${\alpha}$ emission distribution (in grayscale) and T$_c$ (in contours) is displayed in the lower panel. The dust colour temperature distribution was obtained from the $HIRES$ images at 60 and 100 $\mu$m, following the procedure described by @cichowolski01. Derived temperatures correspond to $n$ = 1.5. The parameter $n$ is related to 