Using Cluster magnetic field data, we adopt wavelet analysis and multi-point phase-differencing techniques to study the solar wind turbulence at ion kinetic scales. We are able to determine the power anisotropy in wave-vector space using tens of thousands of wave packets simultaneously observed by four
Cluster spacecraft. Similar to the results of previous k-filtering analysis, we found that the turbulence power is rested in wave vectors dominantly in directions nearly perpendicular to the scale dependent mean magnetic field. The phase-differencing technique further reveals a very weak and quasi-parallel propagating turbulence component, at least in some of the fast solar wind cases we studied. Previous k-
filtering results did not find such weak component. When its presence was revealed by magnetic helicity analysis, the power of the component however was unknown.