We present MUSE observations of the debated ultra faint stellar system Crater . We spectroscopically confirm 26 member stars of this system via radial velocity measurements . We derive the systematic instrumental velocity uncertainty of MUSE spectra to be 2.27 km s ^ { -1 } . This new dataset increases the confirmed member stars of Crater by a factor of 3 . One out of three bright blue stars and a fainter blue star just above the main-sequence-turn-off are also found to be likely members of the system . The observations reveal that Crater has a systemic radial velocity of v _ { sys } = 148.18 ^ { +1.08 } _ { -1.15 } km s ^ { -1 } , whereas the most likely velocity dispersion of this system is \sigma _ { v } = 2.04 ^ { +2.19 } _ { -1.06 } km s ^ { -1 } . The total dynamical mass of the system , assuming dynamical equilibrium is then M _ { tot } = 1.50 ^ { +4.9 } _ { -1.2 } \cdot 10 ^ { 5 } M _ { \odot } implying a mass-to-light ratio of M/L _ { V } =8.52 ^ { +28.0 } _ { -6.5 } M _ { \odot } / L _ { \odot } , which is consistent with a purely baryonic stellar population within its errors and no significant evidence for the presence dark matter was found . We also find evidence for a velocity gradient in the radial velocity distribution . We conclude that our findings strongly support that Crater is a faint intermediate-age outer halo globular cluster and not a dwarf galaxy .