The standard assumption is that the dark matter (DM) density in the early universe can be described by the thermal equilibrium distribution. The DM mass can be therefore determined by the DM interaction with the visible matter in order to fulfill the relic density measured by PLANCK. Consequently, such a DM interaction is not tiny and expected to be found within the detectors. This leads to the main motivation of weakly interacting massive particle (WIMP), one of the most popular DM candidates. However, WIMPs do not appear with the efforts of 30 years searching tasks in various detectors. Instead, the current DM direct detection XENON1T sets a stringent limit on DM interaction. This also discourages the new development of WIMP detectors. In this talk, I will first scrutinize the possible WIMP remaining parameter space and propose several ideas to detect such hidden corners.