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The ever increasing size and complexity of data coming from simulations ofcosmic structure formation demands equally sophisticated tools for theiranalysis. During the past decade, the art of object finding in thesesimulations has hence developed into an important discipline itself. Amultitude of codes based upon a huge variety of methods and techniques havebeen spawned yet the question remained as to whether or not they will providethe same (physical) information about the structures of interest. Here wesummarize and extent previous work of the "halo finder comparison project": weinvestigate in detail the (possible) origin of any deviations across finders.To this extent we decipher and discuss differences in halo finding methods,clearly separating them from the disparity in definitions of halo properties.We observe that different codes not only find different numbers of objectsleading to a scatter of up to 20 per cent in the halo mass and Vmax function,but also that the particulars of those objects that are identified by allfinders differ. The strength of the variation, however, depends on the propertystudied, e.g. the scatter in position, bulk velocity, mass, and the peak valueof the rotation curve is practically below a few per cent, whereas derivedquantities such as spin and shape show larger deviations. Our study indicatesthat the prime contribution to differences in halo properties across codesstems from the distinct particle collection methods and -- to a minor extent --the particular aspects of how the procedure for removing unbound particles isimplemented. We close with a discussion of the relevance and implications ofthe scatter across different codes for other fields such as semi-analyticalgalaxy formation models, gravitational lensing, and observables in general.

Structure Finding in Cosmological Simulations: The State of Affairs