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I discuss two of the possible sources of biases in the determination of theIMF: binning and the existence of unresolved components. The first source isimportant for clusters with a small number of stars detected in a given massbin while the second one is relevant for all clusters located beyond theimmediate solar neighborhood. For both cases I will present results ofnumerical simulations and I will discuss strategies to correct for theireffects. I also present a brief description of a third unrelated bias source.

IMF biases created by binning and unresolved systems