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In recent years, there were studies on the omnipresence and structures offilaments in star-forming regions, and the role of their fragmentation in theprocess of star formation. However, only a few studies analysed the evolutionof filaments and their distribution with the Galactic disk where filaments formself-consistently as part of large-scale molecular cloud evolution. In thisthesis, I perform dust radiative transfer calculations to study the effect ofinclination on dust observations of filaments to evaluate whether thevariations enable the identification of more filaments within dust surveys. Iaddress the early evolution of pc-scale filaments that form within individualclouds and focus on how and when the filaments fragment, and how thefragmentation relates to typically used observables. For evaluating theequilibrium state of filaments and the nature of their fragmentation I examinethree simulated molecular clouds formed in kpc-scale numerical simulationsmodelling a self-gravitating, magnetised, stratified, supernova-driven ISM. Thefirst fragments appear when the line masses of the simulated filaments lie wellbelow the critical line mass of Ostrikers isolated hydrostatic equilibriumsolution. This indicate that, although the turbulence of the entire clouds ismostly driven by gravitational contraction, fragmentation does not occur do togravitational instability, but is supported by colliding flow motions. Iconclude that there is no single quantity in my analysis that can uniquelytrace the inclination and 3D structure of a filament based on dust observationsalone. A simple model of an isolated, isothermal cylinder may not provide agood approach for fragmentation analysis, independently of the dominant drivingsource of the parental cloud.

On Filaments within Molecular Clouds and their Connection to Star Formation