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Aims. This work provides an analysis of how the galaxy number density of theinput data affects the filaments detected with the Bisous filament finder andgives estimates of the reliability of the method itself to assess therobustness of the results.  Methods. We applied the Bisous filament finder to MultiDark-Galaxies data,using various magnitude cuts from the catalogue to study the effects ofdifferent galaxy number densities on the results and different parameters ofthe model. We compared the structures by the fraction of galaxies in filamentsand the volume filled by filaments, and we analysed the similarities betweenthe results from different cuts based on the overlap between detectedfilamentary structures. The filament finder was also applied to the exact samedata 200 times with the same parameters to study the stochasticity of theresults and the correlation between different runs was calculated.  Results. Multiple samples show that galaxies in filaments have preferentiallyhigher luminosity. We found that when a galaxy is in a filament there is a 97%chance that the same galaxy would be in a filament with even more completeinput data and about 85% of filaments are persistent when detecting thefilamentary network with higher-density input data. Lower galaxy number densityinputs mean the Bisous model finds fewer filaments, but the filaments found arepersistent even if we use more complete input data for the detection. Wecalculated the correlation coefficient between 200 Bisous runs on the exactsame input, which is 0.98.  Conclusions. This study confirms that increased number density of galaxies isimportant to obtain a more complete picture of the cosmic web. To overcome thelimitation of the spectroscopic surveys, we will develop the Bisous modelfurther to apply this tool to combined spectroscopic and narrow-bandphotometric redshift surveys, such as the J-PAS.

Assessing the reliability of the Bisous filament finder