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

We briefly summarize the method of simulating Sgr A* polarized sub-mm spectra from the accretion flow and fitting the observed spectrum. The dynamical flow model is based on three-dimensional general relativistic magneto hydrodynamic simulations. Fully self-consistent radiative transfer of polarized cyclo-synchrotron emission is performed. We compile a mean sub-mm spectrum of Sgr A* and fit it with the mean simulated spectra. We estimate the ranges of inclination angle θ=42°-75°, mass accretion rate Ṁ=(1.4-7.0)×10^-8 M _⊙year^-1, and electron temperature T _e =(3-4)×10¹⁰K at 6M. We discuss multiple caveats in dynamical modeling, which must be resolved to make further progress.