We show individual high resolution spectra of components A , B , and C of the nearby late-M type multiple system LHS 1070 . Component A is a mid-M star , B and C are known to have masses at the threshold to brown dwarfs . From our spectra we measure rotation velocities and the mean magnetic field for all three components individually . We find magnetic flux on the order of several kilo-Gauss in all components . The rotation velocities of the two late-M objects B and C are similar ( v \sin { i } = 16 km s ^ { -1 } ) , the earlier A component is spinning only at about half that rate . This suggests weakening of net rotational braking at late-M spectral type , and that the lack of slowly rotating late-M and L dwarfs is real . Furthermore , we found that magnetic flux in the B component is about twice as strong as in component C at similar rotation rate . This indicates that rotational braking is not proportional to magnetic field strength in fully convective objects , and that a different field topology is the reason for the weak braking in low mass objects .