Advances in asteroseismology of solar-like stars , now provide a unique method to estimate the stellar inclination i _ { \star } .
This enables to evaluate the spin-orbit angle of transiting planetary systems , in a complementary fashion to the Rossiter-McLaughlineffect , a well-established method to estimate the projected spin-orbit angle \lambda .
Although the asteroseismic method has been broadly applied to the Kepler data , its reliability has yet to be assessed intensively .
In this work , we evaluate the accuracy of i _ { \star } from asteroseismology of solar-like stars using 3000 simulated power spectra .
We find that the low signal-to-noise ratio of the power spectra induces a systematic under-estimate ( over-estimate ) bias for stars with high ( low ) inclinations .
We derive analytical criteria for the reliable asteroseismic estimate , which indicates that reliable measurements are possible in the range of 20 ^ { \circ } \lesssim i _ { \star } \lesssim 80 ^ { \circ } only for stars with high signal-to-noise ratio .
We also analyse and measure the stellar inclination of 94 Kepler main-sequence solar-like stars , among which 33 are planetary hosts .
According to our reliability criteria , a third of them ( 9 with planets , 22 without ) have accurate stellar inclination .
Comparison of our asteroseismic estimate of v \sin { i _ { \star } } against spectroscopic measurements indicates that the latter suffers from a large uncertainty possibly due to the modeling of macro-turbulence , especially for stars with projected rotation speed v \sin i _ { \star } \lesssim 5 km/s .
This reinforces earlier claims , and the stellar inclination estimated from the combination of measurements from spectroscopy and photometric variation for slowly rotating stars needs to be interpreted with caution .