We develop a detailed methodology of determining three-dimensionally the angle between the stellar spin and the planetary orbit axis vectors , \psi , for transiting planetary systems . The determination of \psi requires the independent estimates of the inclination angles of the stellar spin axis and of the planetary orbital axis with respect to the line-of-sight , i _ { \star } and i _ { orb } , and the projection of the spin–orbit angle onto the plane of the sky , \lambda . These are mainly derived from asteroseismology , transit lightcurve and the Rossiter-McLaughlin effect , respectively . The detailed joint analysis of those three datasets enables an accurate and precise determination of the numerous parameters characterizing the planetary system , in addition to \psi . We demonstrate the power of the joint analysis for the two specific systems , HAT-P-7 and Kepler-25 . HAT-P-7b is the first exoplanet suspected to be a retrograde ( or polar ) planet because of the significant misalignment \lambda \approx 180 ^ { \circ } . Our joint analysis indicates i _ { \star } \approx \timeform { 30 D } and \psi \approx 120 ^ { \circ } , suggesting that the planetary orbit is closer to polar rather than retrograde . Kepler-25 is one of the few multi-transiting planetary systems with measured \lambda , and hosts two short-period transiting planets and one outer non-transiting planet . The projected spin–orbit angle of the larger transiting planet , Kepler-25c , has been measured to be \lambda \approx 0 ^ { \circ } , implying that the system is well-aligned . With the help of the tight constraint from asteroseismology , however , we obtain i _ { \star } = \timeform { 65 D .4 } ^ { + \timeform { 10 D .6 } } _ { - \timeform { 6 D .4 } } and \psi = \timeform { 26 D .9 } ^ { + \timeform { 7 D .0 } } _ { - \timeform { 9 D .2 } } , and thus find that the system is actually mildly misaligned . This is the first detection of the spin–orbit misalignment for the multiple planetary system with a main-sequence host star , and points to mechanisms that tilt a stellar spin axis relative to its protoplanetary disk .