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W51 is a giant radio complex lying along the tangent to the Sagitarius arm ata distance of about 7kpc from Sun, with an extension of about 1deg in the sky.It is divided into three components A,B,C where W51A and W51B consist of manycompact HII regions while W51C is a supernova remnant. We have made continuumradio observations of these HII regions of the W51 complex at 240,610,1060,1400MHz using GMRT with lower resolution 20''x15'' at the lowest frequency. Theobserved spectra of the prominent thermal subcomponents of W51 have been fittedto a free-free emission spectrum and their physical properties like electrontemperatures and emission measures have been estimated. The electrontemperatures from continuum spectra are found to be lower than the temperaturesreported from radio recombination line (RRL) studies of these HII regionsindicating the need for a filling factor even at this resolution. Also, theobserved brightness at 240MHz is found to be higher than expected from the bestfits suggesting the need for a multicomponent model for the region.

Electron temperatures in W51 complex from high resolution, low frequency radio observations