Other sources in the fields

The $\sim1{^\circ}.4$ beam of the GMRT at 327 MHz reveal a number of other compact, moderately resolved and as well as well resolved sources. The 1 arcmin shell type source G003.6$-$0.11, well resolved in the high resolution GMRT image, coincides with significant thermal emission and a H II region. A shell of emission, with three compact source superimposed is clearly visible. Resolved images of this source at 1.4 and 5 GHz were also made using older VLA observations by Gaensler (1999) and Yusef-Zadeh (data obtained from VLA achieves) respectively. Emission from the shell appears to be non-thermal while one of the compact sources is consistent with it being a symbiotic star (Seaquist & Taylor1990). H I absorption observations towards this direction indicate that one of the compact sources and the shell are at similar distances while another compact source is a background object. Earlier, RRL emission has also been detected from this direction at $\sim 5$ GHz, but at a resolution which covers the entire source. Higher resolution continuum and RRL observations with the VLA are required to determine the true nature of this object.

Maps of the field containing G004.2$-$0.0 and G356.3$-$1.5 reveal extended emission, coincident with previously classified UC H II regions. Recently, such extended emission has been detected around a number of UC H II regions using the VLA in D-array configuration (Kim & Koo2001; Kurtz et al.1999). This extended component was not detected earlier since earlier observations were done in the B- or A-array configurations at high frequencies which were insensitive to large scale emission. The GMRT offers a unique advantage in imaging such sources in terms of providing high resolution and simultaneous sensitivity to emission at large scales. Such extended emission, if associated with the UC H II regions, can mitigate the ``age problem'' for these objects (de Pree et al.1995, and reference therein).

A linear structure, seen in the field G356.3$-$1.5, is similar to other linear structures in few other observations in the Galaxy (Gray1996). Higher resolution imaging of this feature is required to determine its physical properties.