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We present a kinematic study of a thousand of dwarf satellites of MW/M31-likehosts from the IllustrisTNG50 simulation. Internal kinematics were derived forall the snapshots to obtain a historical record of their rotation velocity inthe plane of the sky ($|V_T|$) and the amplitude of their velocity gradientsalong the line of sight ($A_{\rm grad}^{v_z}$) measured from the host. For themajority of the satellites we initially detected rotation in the plane of thesky (65%) or velocity gradients (80%), and this was progressively reduced to45% and 68% at $z = 0$ respectively. We find that the evolution of the rotationin the plane of the sky and the velocity gradients differs according to type ofdwarfs, which could be explained in terms of their different masses and orbitalhistories. We observe that interaction with the host has an impact on theevolution of the internal kinematics of the satellites. The rotation signal ofthe satellites is progressively reduced during pericentric passages, the firstpericentre being especially disruptive for the initial kinematics. We observetemporary increases in $A_{\rm grad}^{v_z}$ during pericentric passage causedby tidal interaction with the host, $A_{\rm grad}^{v_z}$ increasing as thesatellites approach their pericentre and dropping as they move away. Insummary, we conclude that the presence of detectable rotation in dwarfsatellites is not uncommon, and that the evolution of their internal kinematicsis clearly affected by their interaction with the host.

Internal kinematics of dwarf satellites of MW/M31-like galaxies in TNG50