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We briefly summarize the method of simulating Sgr A* polarized sub-mm spectrafrom the accretion flow and fitting the observed spectrum. The dynamical flowmodel is based on three-dimensional general relativistic magneto hydrodynamicsimulations. Fully self-consistent radiative transfer of polarizedcyclo-synchrotron emission is performed. We compile a mean sub-mm spectrum ofSgr A* and fit it with the mean simulated spectra. We estimate the ranges ofinclination angle theta=42-75deg, mass accretion rateMdot=(1.4-7.0)*10^{-8}Msun/yr, and electron temperature Te=(3-4)*10^{10}K at6M. We discuss multiple caveats in dynamical modeling, which must be resolvedto make further progress.

Constraining the Accretion Flow in Sgr A* by General Relativistic Dynamical and Polarized Radiative Modeling