![]() ![]() ![]() A quantitative comparison between star and cluster formation is used to study the rapid dispersion, also called infant mortality, of young star clusters. Exploiting different multi-wavelength datasets we compare the positions of current star formation sites and recently formed star clusters younger than 10 Myr. From this we find that the positions of the star clusters show a hierarchy with a fractal dimension similar to that of the turbulent interstellar medium in other galaxies, suggesting that star formation is hierarchical with a universal fractal dimension. ![]() The spatial distribution of the young star clusters is analysed using two-point autocorrelation functions. After considering different scenarios for this object, we conclude that this object is most likely a fuzzy star cluster in front of the disc, with an age of 1.4 Gyr. We discover a peculiar, fuzzy object with a projected position close to the nucleus of M51. The majority of the youngest star clusters are found in the spiral arms and these clusters are slightly more compact compared to older star clusters in the interarm regions. ![]() This suggests that during the formation of star clusters their radii change in a non-uniform way. We determine the radius distribution of 1284 young star clusters, which is different compared to the radius distribution of the giant molecular clouds. By comparing the properties of the young star clusters to the properties of the giant molecular clouds from which they form, we study the process of star formation indirectly. We study how these properties are related and how they depend on different environmental conditions in the galaxy, such as galactocentric radius and the distance from the spiral arms. read more their ages, masses, radii and their spatial distribution. Observations taken by the Hubble Space Telescope in the optical and the near-UV are used to determine fundamental properties of the star clusters, such as. Found in the constellation Canes Venatici, M51 is 37 million light-years away.This thesis presents the results of observational studies of the star cluster population in the interacting spiral galaxy M51, also known as the Whirlpool galaxy. The Whirlpool galaxy is a favorite target for amateur and professional astronomers, alike, and was the first light target for the Infrared Space Observatory. The companion, NGC 5195, was discovered in 1781 by Pierre Mechain. Colloquially, M51 is also known as the "Whirlpool Galaxy", or "Rosse's Galaxy," after Lord Rosse, who first detected galaxy spiral structure in his observations of M51. The Messier catalogue of galaxies is named after him. M51 was one of the original discoveries of Charles Messier, found in October 1773 while he was observing a faint comet. The targeted galaxy is known by various names: M51 from its Messier catalog designation, and also as NGC 5194. A four-color composite, the visible light image shows emissions from 0.4 to 0.7 microns, including the H-alpha nebular feature (red in the image). This visible light view of the spiral galaxy M51 comes from the Kitt Peak National Observatory 2.1m telescope, and measures 9.9 by 13.7 arcminutes (north up). ![]()
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