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Recent developments of the Velocity Gradient Technique (VGT) show that thevelocity gradients provide a reliable tracing of magnetic field direction inturbulent plasmas. In this paper, we explore the ability of velocity gradientsto measure the magnetization of interstellar medium. We demonstrate that thedistribution of velocity gradient orientations provides a reliable estimationof the magnetization of the media. In particular, we determine the relationbetween Alfvenic Mach number $M_A$ in the range of $M_A \in [0.2,1.7]$ andproperties of the velocity gradient distribution, namely, with the dispersionof velocity gradient orientation as well as with the peak to base ratio of theamplitudes. We apply our technique for a selected GALFA-HI region and find theresults consistent with the expected behavior of $M_A$. Using 3D MHDsimulations we successfully compare the results with our new measure ofmagnetization that is based on the dispersion of starlight polarization. Wedemonstrate that, combined with the velocity dispersion along the line of sightdirection, our technique is capable to delivering the magnetic field strength.The new technique opens a way to measure magnetization using other gradientmeasures such as synchrotron intensity gradients (SIGs) and synchrotronpolarization gradients (SPGs).

Distribution of velocity gradient orientations: Mapping magnetization with the Velocity Gradient Technique