Abstract
Since synchrotron polarization fluctuations are related to the fundamental properties of the magnetic field, we propose the polarization intensity variance to measure the Galactic interstellar medium (ISM) magnetization. We confirm the method’s applicability by comparing it with the polarization angle dispersion and its reliability by measuring the underlying Alfvénic Mach number of magnetohydrodynamic turbulence. With the finding of the power-law relation of A∝MA2 between polarization intensity variance A and Alfvénic Mach number M A, we apply the new technique to the Canadian Galactic Plane Survey data, achieving the Alfvénic Mach number of the Galactic ISM. Our results show that the low-latitude Galactic ISM is dominated by sub-Alfénic turbulence, with M A approximately between 0.5 and 1.0.
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