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Filaments represent a key structure during the early stages of the starformation process. Simulations show filamentary structure commonly formedbefore and during the formation of cores. Aims. The Serpens Core represents anideal laboratory to test the state-of-the-art of simulations of turbulent GiantMolecular Clouds. We use Herschel observations of the Serpens Core to computetemperature and column density maps of the region. Among the simulations ofDale et al. (2012), we select the early stages of their Run I, before stellarfeedback is initiated, with similar total mass and physical size as the SerpensCore. We derive temperature and column density maps also from the simulations.The observed distribution of column densities of the filaments has beenanalysed first including and then masking the cores. The same analysis has beenperformed on the simulations as well. A radial network of filaments has beendetected in the Serpens Core. The analysed simulation shows a strikingmorphological resemblance to the observed structures. The column densitydistribution of simulated filaments without cores shows only a log-normaldistribution, while the observed filaments show a power-law tail. The power-lawtail becomes evident in the simulation if one focuses just on the columndensity distribution of the cores. In contrast, the observed cores show a flatdistribution. Even though the simulated and observed filaments are subjectivelysimilar-looking, we find that they behave in very different ways. The simulatedfilaments are turbulence-dominated regions, the observed filaments are insteadself-gravitating structures that will probably fragment into cores.

A network of filaments detected by Herschel in the Serpens Core: A laboratory to test simulations of low-mass star formation