We use a set of magnetohydrodynamics ( MHD ) simulations of fully-developed ( driven ) turbulence to study the anisotropy in the velocity field that is induced by the presence of the magnetic field .
In our models we study turbulence characterized by sonic Mach numbers M _ { s } from 0.7 to 7.5 , and Alfvén Mach numbers from 0.4 to 7.7 .
These are used to produce synthetic observations ( centroid maps ) that are analyzed .
To study the effect of large scale density fluctuations and of white noise we have modified the density fields and obtained new centroid maps , which are analyzed .
We show that restricting the range of scales at which the anisotropy is measured makes the method robust against such fluctuations .
We show that the anisotropy in the structure function of the maps reveals the direction of the magnetic field for M _ { A } \lesssim 1.5 , regardless of the sonic Mach number .
We found that the degree of anisotropy can be used to determine the degree of magnetization ( i.e . M _ { A } ) for M _ { A } \lesssim 1.5 .
To do this , one needs an additional measure of the sonic Mach number and an estimate of the LOS magnetic field , both feasible by other techniques , offering a new opportunity to study the magnetization state of the interstellar medium .