Astrophysical and cosmological observations from galactic to cosmological scales indicate the existence of dark matter. Nevertheless, most of its property still remain to be unknown and hence candidates range from 10^-31 to 10^50 GeV in its mass scale. Among them, the traditional dark matter candidate, so called WIMP (weakly interacting massive particle) is still attractive because its production mechanism, i.e., thermal freeze-out, naturally explains its abundance and pins down its mass scale to be 1 ~ 10^5 GeV. Moreover, the same interaction required for the thermal freeze-out allows us to detect them directly/indirectly. The key observable for this program is the abundance of dark matter, which is one exceptional parameter we measured very precisely, i.e., within 1% accuracy. Hence, it is desirable to give theoretical prediction of WIMP abundance for a given model within this accuracy. Based on these, I will talk about my recent attempts to refine the calculation of WIMP abundance.
Peter Thirolf (LMU) / Norbert Kaiser (TUM)