Knowledge of Jupiter ’ s deep interior would provide unique constraints on the formation of the Solar System .
Measurement of its core mass and global composition would shed light on whether the planet formed by accretion or by direct gravitational collapse .
At present , the inner structure of Jupiter is poorly constrained and seismology , which consists of identifying acoustic eigenmodes , offers a way to directly measure its deep sound speed profile , and thus its physical properties .
Seismology of Jupiter has been considered since the mid 1970s , but hitherto the various attempts to detect global modes led , at best , to ambiguous results .
We report the detection of global modes of Jupiter , based on radial velocity measurements performed with the SYMPA Fourier spectro-imager .
The global seismic parameters that we measure include the frequency of maximum amplitude 1213 \pm 50 \mu Hz , the mean large frequency spacing between radial harmonics 155.3 \pm 2.2 \mu Hz and the mode maximum amplitude 49 _ { -10 } ^ { +8 } cm s ^ { -1 } , all values that are consistent with current models of Jupiter .
This result opens the way to the investigation of the inner structure of the Solar System ’ s giant planets based on seismology techniques .