This work presents a preliminary study on the distribution of intensity in stellar absorption lines, focusing on quantitative observations of broad and strong lines in the spectra of various stars. It discusses the methodology employed, including the use of objective prism spectra and microphotometry for analysis. The research highlights the significance of absorption line contours in understanding atomic structure and the physical constitution of stellar atmospheres. The findings are based on a series of spectrograms obtained from different stars, detailing the techniques used to ensure accurate measurements and the challenges faced during the analysis.