{'fraction_non_alphanumeric': 0.02158273381294964, 'fraction_numerical': 0.0341726618705036, 'mean_word_length': 4.888888888888889, 'pattern_counts': {'":': 0, '<': 0, '<?xml version=': 0, '>': 0, 'https://': 0, 'lorem ipsum': 0, 'www.': 0, 'xml': 0}, 'pii_count': 0, 'substrings_counts': 0, 'word_list_counts': {'cursed_substrings.json': 0, 'profanity_word_list.json': 0, 'sexual_word_list.json': 0, 'zh_pornsignals.json': 0}}
Low Frequency Radio Observations Of W51 Complex

W51 is a giant radio complex lying along the tangent to the Saggitarius arm at a distance of about 7kpc from Sun, with an extension of about 1◦ in the sky. It is divided into three components A,B,C where W51A and W51B are regions consisting of many compact HII sources.We have made continuum radio observations of these HII regions of W51 complex at 240,610,1060,1400 MHz frequencies using GMRT. The observed spectrum for each of the prominent subcomponents of W51A, G49.5-0.4 and G49.4-0.3 has been obtained by least-square fitting of flux and frequency to free-free emission spectrum and physical properties like electron temperature and emission measure have been derived from it for each of the discrete sources. Electron temperatures, estimated from continuum spectrum, are found to be low and different from the temperatures reported from RRL studies of these HII regions. We propose a simple two component model to account for the apparent discrepancy between RRL temperature and electron temperature obtained from fit including higher frequencies as well.