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This study proceeds with the development of the technique employing velocitygradients that were identified in (\cite{GL17}, henceforth GL17) as a means ofprobing magnetic field in interstellar media. We demonstrate a number ofpractical ways on improving the accuracy of tracing magnetic fields in diffuseinterstellar media using velocity centroid gradients (VCGs). Addressing themagnetic field tracing in super-Alfvenic turbulence we introduce the procedureof filtering low spatial frequencies, that enables magnetic field tracing inthe situations when the kinetic energy of turbulent plasmas dominate itsmagnetic energy. We propose the synergic way of of using VCGs together withintensity gradients (IGs), synchrotron intensity gradients (SIGs) as well asdust polarimetry. We show that while the IGs trace magnetic field worse thanthe VCGs, the deviations of the angle between the IGs and VCGs trace the shocksin diffuse media. Similarly the perpendicular orientation of the VCGs and theSIGs or to the dust polarimetry data trace the regions of gravitationalcollapse. We demonstrate the utility of combining the VCGs, IGs and polarimetryusing GALFA HI and Planck polarimetry data. We also provide an example ofsynergy of the VCGs and the SIGs using the HI4PI full-sky HI survey togetherwith the Planck synchrotron intensity data.

Tracing interstellar magnetic field using the velocity gradient technique in shock and self-gravitating media