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Polarimetry is extensively used as a tool to trace the interstellar magneticfield projected on the plane of sky. Moreover, it is also possible to estimatethe magnetic field intensity from polarimetric maps based on theChandrasekhar-Fermi method. In this work, we present results for turbulent,isothermal, 3-D simulations of sub/supersonic and sub/super-Alfvenic cases.With the cubes, assuming perfect grain alignment, we created syntheticpolarimetric maps for different orientations of the mean magnetic field withrespect to the line of sight (LOS). We show that the dispersion of thepolarization angle depends on the angle of the mean magnetic field regardingthe LOS and on the Alfvenic Mach number. However, the second order structurefunction of the polarization angle follows the relation $SF \proptol^{\alpha}$, $\alpha$ being dependent exclusively on the Alfvenic Mach number.The results show an anti-correlation between the polarization degree and thecolumn density, with exponent $\gamma \sim -0.5$, in agreement withobservations, which is explained by the increase in the dispersion of thepolarization angle along the LOS within denser regions. However, this effectwas observed exclusively on supersonic, but sub-Alfvenic, simulations. For thesuper-Alfvenic, and the subsonic model, the polarization degree showed to beintependent on the column density. Our major quantitative result is ageneralized equation for the CF method, which allowed us to determine themagnetic field strength from the polarization maps with errors $< 20%$. We alsoaccount for the role of observational resolution on the CF method.

Studies of regular and random magnetic fields in the ISM: statistics of polarization vectors and the Chandrasekhar-Fermi technique