Multiwavelength observations of the HII region of NGC 6357

In this thesis, I conducted an analysis of the emissions originating from the NGC 6357, also known as the Lobster Nebula. This nebula exhibits emissions within radio frequency bands. Through observations with ALMA, the J=1-0 emission of Hydrogen Cyanide (HCN), a molecule that traces high-density gas, were successfully detected and identified. Through an examination of these emission lines, I derived some parameters of the source like temperature, column density, and mass. Subsequently, I embarked on a phase aimed at expanding the scope of observations for NGC 6357 by exploring various wavelengths. Specifically, I conducted an analysis of observations in the WISE W1 (3.4 μm), W2(4.6 μm), and W3(12 μm) bands, which are included in the AllWise catalog. This endeavor was taken in an effort to establish potential correlations with the HCN emission regions. I found that these HCN emission areas indeed represent pre-main sequence regions. This conclusion agrees with the characteristics extracted from ALMA observations. This study demonstrates that the HCN emissions observed with ALMA in NGC 6357 originate from pre-main sequence sources, particularly prestellar cores. These sources exhibit temperatures spanning the range from 10 to 30 K and are characterized by high column densities. These findings contribute significantly to our broader comprehension of star-forming regions of NGC 6357.